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The NAM Local Organising Committee would like to thank the following organisations for their generous support of

NAM 2010

National Astronomy Meeting

Abstracts Book

2010 April 12–16

http://www.astro.gla.ac.uk/nam2010/

National Astronomy Meeting

Abstracts Book

2010 April 12–16

ContentsWelcome! 2

Acknowledgements 4SocialEvents 5

Outreachevents 6Localinformation 7

Sessions 14RAS Afternoon 40

Abstracts 42IndexofAuthors 91

Listofparticipants 97

Wel

com

e! AndyFabian

As President of the Royal AstronomicalSociety(RAS),itgivesmegreatpleasuretowelcomeyoutoGlasgowUniversityforthe2010RAS NationalAstronomyMeet-ing, the UK’s largest annual astronomyandspacescienceevent. Morethan500scientists are registered for theMeeting,frompostgraduate students to senior re-searchersandacademicstaff. Duringtheweek, wewilldiscussandpresentcutting-edgesciencefromacrossourfield, fromthe upper atmosphere of the Earth togalaxiesintheearlyUniverse. IntheUKwearenotonlyoutstandinginourfield,rankingsecondto theUS,butoutstand-ingatcommunicatingourwork. Astron-omy’sprofileinthemediaishigherthanever, hasanenduringpopularitywithstudents inour schoolsand iscitedbymanyasakeyfactorforinspiringentryintoacareerinscience. SoatNAM2010wecancelebratethebestofourscienceinaninstitutionwhereastronomyhasbeentaughtforhalfamillennium, andresearchedindepthsincethe1760ap-pointmentofAlexanderWilsonas thefirstRegiusChairofAstronomy, rightlycelebratedinthis250thanniversaryyear. Glasgowisagreatplaceforouran-nualMeetingtotakeplaceandwhateveryourareaofworkI hopetoseeandtalktomanyofyouinthedaysahead.

AndyFabian, PresidentoftheRoyalAstronomicalSociety

JohnC Brown

OnbehalfoftheLOC,SOC andalllocalGlasgow area astronomers, professionalandamateur, I extend toallNAM 2010delegates a verywarmwelcome to ourfinecityandtotheGU CampusNAM site.WealsowishtothankRAS/NAM forac-ceptingourinvitationtothissiteinrecog-nition of the 250th Anniversary of ourRegiusChairofAstronomy. Solarphysics,MIST andAstronomyhaveundergonead-vancesunimaginableinWilson’sdayandastonishingeven since the lastGlasgowNAM (thenanRAS OutofTownMeeting)in1989. Enjoyallthelatestsciencenewsherebut alsomake sure you take sometimetoenjoyourcity, environs, andleg-endaryhospitality

JohnC Brown, 10thRegiusChairofAs-tronomyand10thAstronomerRoyal forScotland

250yearsoftheRegiusChairofAstronomyinGlasgow: AlexanderWilson, firstRegiusChair

Alexander Wilson MA, MD was thefirstappointee(1760-1784)totheRegiusChairofPracticalAstronomy, Universityof Glasgow (founded 1451). This fol-lowedestablishmentofthefirstdedicatedUniversity Observatory in 1757, basedon an instrument collection donated byAlexander McFarlane of Jamaica. Re-furbishmentoftheinstrumentsaftertheirdeleterious voyagewere carried out for£5byJamesWatt, atthattimea19yearoldUniversity instrumentmaker. TherehavebeentenRegiusChairstodate, thecurrentincumbent, JohnC Brown, beingalso10thAstronomerRoyalforScotland.

Born in St Andrews, Wilson graduatedMA (1733)thereandbecameanappren-ticetoaLondonsurgeonandapothecary. HereturnedtoStAndrewsin1739tostarta type foundrybusinesswhichmoved toGlasgowin1744, supplyingtheUniversity printers. In business partnershipwith JamesWatt and JosephBlack, hemade some of the earliest scientific thermometerswhich played acentralroleinBlack’sworkontheoriesoflatentandspecificheat. PriortohisChair appointment, Wilsonhad invented a newprocess for type, made tele-scopes, flownthermometersonkites, andmadespecificgravitybeadsforliq-uid testing includingspirit ‘proof’ strength. WhileRegiusChairhewasClerkofSenateand foundermemberof theRoyalSocietyofEdinburgh, aswellasbeing very active in several areas of research, most famously for his obser-vational discovery [Philosophical Transactions (1683–1775), 64:1–30 (1774),doi:10.1098/rstl.1774.0001, ADS:1774RSPT...64....1W] oftheapparentdepres-sionofsunspotsbelowthephotosphere, todaytermedtheWilsonEffect.

[ImageofWilsoncourtesyof JamesBabingtonSmith, Wilsondescendant; ex-cerptsofWilsonpapercourtesyoftheRoyalSociety]

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Ack

now

ledg

emen

ts The LocalOrganising Committee Lyndsay Fletcher (LOC chair), John Brown(LOC DeputyChair), RachaelMcLauchlan(Secretary), MatthewCartmell(De-partmentofMechanicalEngineering), SaraDiegoli(ScottishUniversitiesPhysicsAlliance), DeclanDiver, HelenFraser(UniversityofStrathclyde), NormanGray,GilesHammond, IainHannah, IkSiongHeng, NicLabrosse, AlecMacKinnon(DepartmentofAdultandContinuingEducation), PeterMurray, MattPitkin, Bon-nieSteves(GlasgowCaledonianUniversity), GrahamWoan.

TheScientificOrganisingCommittee MartinHendry(SOC Chair), JohnBrown,EduardKontar(UKSP SOC chair), AnnetteFerguson(ROE IfA,UniversityofEdin-burgh), WayneHolland(UKATC,UniversityofEdinburgh), AndyTaylor(ROE IfA,UniversityofEdinburgh), AlanThompson(BGS Edinburgh, MIST SOC chair), IanBonnell(UniversityofSt. Andrews), JaneGreaves(UniversityofSt. Andrews),SheilaRowan(UniversityofGlasgow).

TheUKSP SOC GerryDoyle (Armagh), Rekha Jain (Sheffield,) EduardKontar(Glasgow; chair), DuncanMacKay(StAndrews), DavidPontin(Dundee).

TheMIST Council

Allofthe sessionconvenors forputtingtogethersuchanexcellentscientificpro-gramme.

OurteamofNAM helpers MattAbernathy, MarinaBattaglia, RiccardoBassiri,Euan Bennet, Nicola Beveridge, Christina Burge, Paul Campsie, EwanDick-son, MattEdgar, HodaGhodsi, ColinGill, DavidGraham, JingnanGuo, KarenHaughian, ErinMacdonald, ProchetaMallik, HeatherRatcliffe, HamishReid,SatoruSakai, IgnacioSantiago, EdwardThomson, FraserWatson.

JohnBrown, LucieGreen, ChrisLintott, FionaSpeirits, FredWatson, and JimWildasoutreacheventpresenters.

FredWatson, MarnieOgg, TheGlasgowSkepticsandTheAdmiralBar(‘ScienceinthePub’).

Alltheschoolswhoparticipatedintheschools’postersession.

Wewouldalsoliketothankthefollowinginthe UniversityofGlasgow fortheirhelpandadvice: IshbelDuncanandLucindaHay(TheConferenceandVisitorServicesOffice), ChaHannawayandBillYoung (AV and IT), EllenThompson(HospitalityServices), PatrickNwaozuzu(FInanceandPurchasingOffice), Stu-artForsyth (CorporateCommunications), AnnePlissiand JacquelineHeuchan(PhysicsandAstronomyAccountsOffice), AlanBowman(PhysicsandAstron-omyStores).

ThankstoIainHannahfortheimageoftheGlasgowUniversityCloistersusedonourAbstractBookandbanners.

Social Events

Monday12thApril

Reception: GlasgowCityChambers ThemeetingreceptionwillbehostedbyGlasgowCityCouncil in theCityChambers, situated in theheart of the citycentre. Thisreceptionincludesdrinksandcanapés. Advancedreservationwasrequired: youwillneedtoshowyourconferencebadgetoenter.

Thisisexpectedtorunfrom18.30to20.00.

ScienceinthePub: TheAdmiralBar A “ScienceinthePub”Q&A panelses-sion, ledbyFredWatsonofAAO,isplannedforMonday12thfrom20.30–23.00directlyaftertheCivicReception. FredWatsonmakesfrequentappearancesonAustralian radio andTV,which, togetherwithhis books, public lectures andastronomytourismexpeditions, haveresultedinseveralawards.

ThevenuewillbetheTheAdmiralBarintheCityCentre, abouta10/15minwalkfromtheCityChambers(Googledirections). ThevenueisaregularhauntofGlasgowSkepticsinthePubwhoarekindlyassistingwiththatevent. Advancedregistrationwasrequired, andalightbuffetwillbeprovidedforthosewhodidregister: showyourconferencebadgetoenter.

Tuesday13thApril

5-a-sideFootball: KelvinhallInternationalSportsArena Thisyear’scompetitionwilloccurindoorsinasportingvenuethathasheldmanyaninternationalsport-ingevent, theKelvinhall, justafewmomentswalkfromtheUniversity.

Thecompetitionisexpectedtorunfrom18.30to21.00.

Wednesday14thApril

Dinner&Ceilidh: KelvingroveArtGalleryandMuseum ThemeetingdinnerwillbefollowedbyatraditionalceilidhbothinthespectacularKelvingroveArtgalleryandMuseum, situatedjustdownthehillfromtheUniversity.

Pleasebringyourconferencebadge, whichalsoshowsthemenuchoiceswhichyoumadeatregistration.

Thedinnerisexpectedtorunfrom19.00to24.00.

Hubble3D previewatGlasgowScienceCentreIMAX

TheGlasgowScienceCentreisshowingthenewHubble3D IMAX film, andtheirprevieweventhasfallenonthe14th. Theyhavekindlyoffered100ticketsforNAMdelegates, soifyouareunabletogototheconferencedinner, thisisanotheralternative. Email SharonLyons (sharon.lyons@glasgowsciencecentre.org) assoonaspossible, ifyouwanttobookaticket.

Youcanfindamapoftheselocationsat http://bit.ly/9v6jsq

Allweek

While inGlasgowmake sure tovisit theGlasgowScienceCentre, whohavespecialratesforNAM delegates. Seepage 9 fordetails.

Out

reac

h ev

ents Publicastronomytalks

Thesetalksarefreetoattend, butifyouhavenotalreadydoneso, pleasereserveafreee-ticketontheweb, at http://www.astro.gla.ac.uk/nam2010/pub.php. Allthetalkswilltakeplaceat19.30inlecturetheatre 257oftheKelvinBuilding,DepartmentofPhysicsandAstronomy, oncampusnexttothemainUniversitybuilding.

19:30Tuesday13thApril2010: TheMagicoftheSunandStars

JohnBrown (UniversityofGlasgow, andAstronomerRoyalforScotland) &LucieGreen (MullardSpaceScienceLaboratory). ExplorethewondersofourownSunandcountlessotherstarsthroughouttheuniverse.

19:30Wednesday14thApril2010: HowtoUseaMillionAstronomers–TheGalaxyZooandBeyond

ChrisLintott (UniversityofOxfordand“TheSkyatNight”). Discoverhow“Cit-izenScientists”arehelpingtounravelthemysteriesofhowgalaxiesformed.

19:30Thursday15thApril2010: HereistheSpaceWeather

JimWild (LancasterUniversity). Learnaboutthespaceenvironmentandhowits“weather”impactsonhumantechnology. InassociationwiththeAstronomicalSocietyofGlasgow, http://www.theasg.org.uk/

JohnBrown&LucieGreen ChrisLintott JimWild

250yearsoftheAstronomyChairatGlasgow

TheHunterianMuseum, nexttothePlenarysessions, willbehostingadisplayonAlexanderWilson. ThereisalsothechanceforasmallnumberofinteresteddelegatestoviewrelatedhistoricalmaterialsfromtheUniversityLibrary’sSpecialCollection(Wednesday14thatlunchtimeandintheafternoon–signupattheregistrationdesk).

Outreach

FridayoftheNAM willincludeaspecialschoolspostersession, from12.00to14.00in theKelvinBuilding(DepartmentofPhysicsandAstronomy). Duringtheweeksprior to themeeting, schoolpupils from thecouncilareasofWestDunbartonshire and South Lanarkshire havebeen researching sunspots, solaractivityandthepressingquestionofanylinkbetweentheseandterrestrialclimate–onethatwouldhaveinterestedAlexanderWilsonhimself. Inthispostersessiontheywillpresenttheirresults. Wehopethatmanyconferenceattendeeswilltaketheopportunitytopopinanddiscusstheireffortsandconclusionswiththem.

Local information

For a link-rich version of this information, see http://www.astro.gla.ac.uk/nam2010/out.php

ThereisahugenumberofplacesinGlasgowtoshop, visit, eat, drink, and/ordance. Sothefollowinglistisbynomeanscomprehensive, butpointstodifferentareasofinterestandwhatyoushouldfindthere.

TheWestEnd(G12)

ByresRoad isthemainstreetforshops, banks, restaurants, barsandpubsintheWestEndandis justa fewminuteswalkwestonUniversityAvenuefromthemainbuildingandNAM2010. ItalsocontainstheHillheadsubwaystop.

Subway HillheadShops Waitrose, Tesco, M&S SimplyFood, Iceland, Peckham’s, ClintonCards,

Clarks, Fopp, Superdrug, Specsavers, PapyrusPharmacy Boots

Banks/BuildingSocities RBS,HBOS,LloydsTSB,Clydesdale, Nationwide, San-tander

Take-a-away UniversityCafe, Starbucks, Subway, LittleItaly, Peckham’s, Gregg’s,HeartBuchanan, BaguetteExpress

Restaurants Paperino’s, OranMor, Balbir’s, Stravaign, theBothy, theTwoFigsPubs/Bars Tennents, OranMor, Aragon, CommonRoom

AshtonLane/CresswellLane isacobbledlanelinedbybarsandrestaurantsthatrunsparalleltoByresRoad, behindHillheadunderground.

Cinema GrosvenorFood&Drink UbiquitousChip(andthePubupstairs), Brel, theLoft, CafeAn-

daluzandmanymore

GreatWesternRoad isatthetopofByresRdandheadseastwardsintothectycentre(withvariousshopsandpubs)andwestwardintotheA82andthehigh-lands. AtthecornerofByresRdandGreatWesternRdistheBotanicGardenswithfreeentrytotherestoredKibblePalaceglasshouse.

Subway KelvinbridgeRestaurants CailBruichWest, TheBigBlue, Gambrino, WudonPubs/Bars OranMor, Coopers, TheBelle, TheWiseMonkey

WoodlandsRdandGibsonSt leadingoffoftheeastofUnivesityAvenue)featuresmoreplacestoeatanddrink.

ComedyClub TheStandPubs/Bars UisgeBeathe, DoubletBar, ThePrimaryRestaurants TheLeftBank, ChilliesWestEnd, TattieMac’s(OtagoSt)

DumbartonRd/SauchiehallSt/ArgyleSt(G3)

DumbartonRd isatthebottomofByresRd. GoingeastwarditsplitsintoArgyleStandSauchiehallStattheKelvingroveArtGallery. BothofthesestreetsendupbeingtwoofthemainshoppingstreetsintheCityCentre.

KelvingroveArtGalleriesandMuseum iscompletely free andawanderaboutisstrongly recommended. ItisthemostpopularfreevisitorattractioninScotlandandmostvisitedUK museumoutsideLondon. Ithasavarietyofexhibits(includ-ingtheobligatorydinosaurs, egyptiansarcophagi, armourandCharlesRennieMackintosh)andfamouspaintingsfromartistsincludingRembrandt, Matisse, Pi-casso, Monet, vanGogh, andparticularlySalvadorDali'sfamousChristofSaintJohnoftheCross. Andofcoursetheconferencedinnerandceilidhwillbethere.

MuseumofTransport isalso free. Itwillbeclosingforever(movingtoanewClydesidemuseumin2011)onthe19thofApril, sothereisaseriesofeventstakingplaceduringtheweekofNAM2010. Withtrams, trainsandships, thisplaceisabigkid’sdelight.

Subway Kelvinhall, PartickFood&Drinks TheGoat, BigSlope, TheSisters, Mother India (+Cafe), Fanny

Trollope’sPubs TheThreeJudges, Lismore, BenNevis

CityCentre

ThemainshoppingstreetinGlasgowareBuchananSt, SauchiehallSt(atthetopofBuchananSt)andArgyleSt(atthebottomofBuchananSt).

Thereisaconcentrationofpubsandrestaurantsinthe MerchantCity, particu-larlyMerchantSquare/Candleriggs (afewblocksoutheastofthecitychambers)

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Subway BuchananSt, StEnochFood&Drinks TheButterfly&thePig, TwoFatLadies, 13thNote(Veggie), Stereo,

Rumours, TheDhabba, OkoExpress,Pubs the(legendary)HorseshoeBar, theLab, CountingHouse(bigWetherspoon’s

acrossfromcitychambers), O’Henry’s

Other

GlasgowScienceCentre/Hubble3D IMAXWhilstinGlasgow, makesuretovisitthe GlasgowScienceCentre (GSC),currentlyhometotheIYA’s‘ExplorersoftheUniverse’photographicexhibition, averyfineplanetarium, andahugeIMAXscreenshowingtheamazingIMAX 3D film‘Hubble’(thisstartsonApril15th,andyoucanbookfreeticketsforapreviewonthe14th–seepage 5 fordetails).TheScienceCentreisalsohostinganamazingexhibition‘WallaceandGromitpresentaWorldofCracking Ideas’whichexplores themesof innovationandinventionaswellasofferingaglimpseintoWallace’szanycreativeworld. AsadelegatetoNAM youwillbenefitfromaspecialdelegaterateof£4perpersonforadmissiontothemainScienceMallonproductionofyourdelegatebadgeattheScienceCentreticketdesk.

TheGSC islocatedonthesouthsideoftheClyde, 40minuteswalkfromthecampus, ortakeataxitotheCrownePlazahotelbytheSECC,andwalkacrossoneofthepedestrianbridges.

Balloch/LochLomond&theHighlands Balloch, thetownatthesouthernedgeofLochLomond, islessthananhourawaybytrainfromQueenStlowlevelrailstation, whichyoucanreachfromPartickstation. TofullyexploreLochLomondandthespectacularhighlandswerecommendacar. GreatWesternRoad, atthetopofByresRoadistheA82andthisoneroadtakesyoutoLochLomond, upbyRannochMoor, Glencoe(under2hoursdriveaway)thenontoFortWilliam,LochNessandeventuallyInverness(about4hoursdrive).

CarRental: Therearenocarhirelocationsconvenientfortheuniversity. Eithergetthecarattheairport(GlasgoworPrestwick)ortheEnterprise(40OswaldSt,G14PL) nexttoCentralstationinthecitycentre.

Stirling&GlengoyneDistillery[Saturday17thApril] Advancedregistrationwasrequiredforthistrip.

FromGlasgowwedriveto themedievalcityofStirlingtovisitStirlingCastle,whichoverlookstheancientcityofStirlingandisoneofthehistoricbuildingsthathavecometosymbolisethespiritofScotland. WecontinuetoTheTrossachsalongtheshoreofLochVenacharthenclimbthedramaticDukesPasstotheprettyvillageofAberfoyle. TheQueenofScotland’slakes-LochLomond-issuretoputasonginyourheart! LochLomondisthelargeststretchofinlandwaterinBritain. We'llmakeastopatLochLomondShoreswhereyoucanenjoy thespectacularscenerybeforeourlaststopofthedayistoprettyGlengoyneMaltWhiskyDistillerywhere, aswellashavingabehindthescenestourtolearnallaboutthedistillersart, therewillbeachancetotastethefinishedproduct!

Eatingoutinthewestend

TheList isanindependentlimitedcompanybasedinScotlandfounded, inOc-tober1985topromotethewiderangeofarts, eventsandentertainmenttakingplaceeachyearinScotland. Thecompanymaintainstheawardwinningweb-site www.list.co.uk, wheredetailedandwide-rangingreviewsoftheeatinganddrinkingsectorinScotlandcanbefound. Belowwehavereproduced(withkindpermission)extractsfromtheList'sguidetoeatingoutinGlasgow'sWestEnd.Seealso http://www.list.co.uk/places/restaurants/where:g12/

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Key: B -Budget; S -StudentFriendly; V -vegetarianoptionsaccountfor1/4ofmenu; W -wi-fi; L -latedining. H -HitList

AshokaAshtonLane (L,V) 19AshtonLaneGlasgow, G128SJ,Foodserved: Mon–Thunoon–midnight; Fri/Satnoon–1am; Sun5pm–midnight. Capacity: 68.TheAshtonLanebranchisperhapsAshoka’smostdesirableoutlet, situatedintheheartoftheWestEnd’squaint, cobbledeatinganddrinkingstripanddecoratedinshadesofcoolorangeandbrownwithalargecolourfulmuralofanIndianstreetscenecoveringonewall. Thefoodisyourtypicalmixofclassiccurries, dosasandtandooris(there’snotahugeamountofdifferencemenu-wiserestauranttorestaurantacrossthechain). It’sallwellcooked, inexpensiveandplentifulstuff,withafewScottishtwistssuchashaggispakora.

TheBigBlue (B,S,V) 445GreatWesternRoad, Glasgow, G128HH,Foodserved: Mon–Thu&Sunnoon–10pm; Fri/Satnoon–10.30pm. Capacity: 56.A spaciouspatiowithrelaxingviewsovertheriverKelvin, Mediterranean-styleinteriorswithtwistedirondécor, bleachedwallsandastylishbar, BigBluere-mainsafunkyhang-outforcitydwellersofallages. ThemenucoverseverybasefromburgerstosteaktopastatoTexMextopizza.

Brel (S) 9–43Ashton Lane, GlasgowG128SG,Foodserved: Mon–Sunnoon–10pm.Capacity: 60.BelgianbarandrestaurantBrelhasbeenafixtureontheWestEnd‚squaintAshtonLane forover12years. Downstairs, thewhite tiledwallsandheavywoodendoors(whichareopenedonwarmdays), givethemainrestaurant–aconvertedstable–arusticfeel. Upstairs, theatmosphericwinebarSergeisanappealingspotforanafterdarkquaffandlightbitebyflickeringcandlelight.

Budda (B,S,V) 8CresswellLane, Glasgow, G128AA,Foodserved: Mon–Satnoon–10pm;Sun12.30–10pm. Capacity: 250.Lodgedon the cobbles of theWest End’sCresswell Lane, BarBuddahas es-tablisheditselfasasports-bar-come-restaurantand, morerecently, alate-nightfoodhaunt. Servinguphigh-qualitypubfooduntil2amattheweekends, Buddaboastsamenuofmostlyburgers, pizzasandsandwiches.

CaféAndaluz (B, L,V) 2CresswellLane, Glasgow, G128AA,Mon–Satnoon–11pm;Sun12.30–10.30pm. Capacity: 130.CaféAndaluz resonateswith aNorthAfrican feel viaMoorish decor. Goodseafood.

CaféAntipasti (B,V) 337ByresRoad, Glasgow, G128UQ,Sun–Thu9am–11pm; Fri/Sat9am–midnight. Capacity: 50.Between the fairy lightsand rusticpine tablesandfittings, youmightbe sur-prisedonfirstimpressionstolearnthatCaféAntipastionByresRoadisanItalianrestaurant. Good, unpretentiousfood.

Chow (B,L) 98ByresRoad, Glasgow, G128TB,Foodserved: Mon–Thunoon–2.15pm,5–11.30pm; Fri/Satnoon–2.15pm, 5pm–midnight; Sun4.30–11.30pm. Capacity: 45.ChowdoesnotfeellikeyouraverageChineserestaurant. Itsmanyregularsprizethefriendlyneighbourhoodvibeandpared-downmoderndécor-andthefood’sfarfromaveragetoo. Canfeelcrowded, though.

DiMaggio’s (B,L) 61RuthvenLane, Glasgow, G129BG,Foodserved: Sun–Thunoon–10.30pm;Fri/Satnoon–11.30pm. Capacity: 125.

Kember&Jones (B,V) 134ByresRoad, Glasgow, G128TD,Mon–Fri8am–9pm; Sat9am–9pm; Sun9am–5pm. Capacity: 36.Kember&JonescallsitselfaFineFoodEmporiumwithoutexaggeration–thisroomycaféandcontinentaldeli reallydoes stock someof the freshest, high-qualitybreakfast, lunch, dinnerandsnackeatsyou’llfindinGlasgow.

Koh-i-Noor (L) 12GibsonStreet, Glasgow, G128NX., Foodserved: Sun–Wednoon–1am;Thu–Satnoon–3am.

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There’salarge, classicIndianmenu, withburgersandkebabstoo. Onceordersareplacedit’snicetobeabletopeerbeyondthecounterandseeamealbeingpreparedwithskillandcare. Punjabimasalaistypical: aclean, creamyheatfromthesauce, ahintofcumin.

TheLeftBank (B,S,V) 33–35GibsonStreet, Glasgow, G128NU,Foodserved: Mon–Fri9am–10pm; Sat/Sun10am–10pm. Capacity: 60.TheLeftBankboastsalltheunderstatedcoolofabarkitchenwhileatthesametimeremainingasrelaxedandversatileasacafébar. ExtensiveVeganoptions.

Mezzo@TheLoft (S) TheGrosvenorTheatre,AshtonLane, Glasgow, G128SJ ,Foodserved: Mon–Satnoon–10pm; Sun11am–10pm. Capacity: 120.A barn-likespaceabovetheGrosvenorCinema, theupstairsrestauranthasnowbeenrevampedwitharusticItaliantheme, withanambitiousmenuemphasisingpeasantdishes, cookedfamily-style(andtheyencouragethemtobesharedthatwaytoo).

NakedSoup (B) 6KerslandStreet, Glasgow, G126BL,Foodserved: Mon–Fri8.30am–8pm;Sat10am–6pm; Sun11am–6pm. Capacity: 20.AlthoughNakedSouphasawiderangeoffoodoptionsonitsmenuincludingasandwiches, saladsandbreakfast, theclueisinthename: thisplacedoesexactlywhatitsaysonthetin.

ÒranMór (B, S) 731–735 GreatWestern Road, Glasgow, G12 8QX, Food served:Mon–Sat9am–9pm; Sun12.30–9pm. Capacity: 140.ThegrandlookingÒranMór, aconvertedsandstonechurchoverlookingByresRoadandtheBotanicGardens, attemptstocaterforthevariedwantsoftrendyWestEndlocalsbybeingallthingstoallpunters: restaurant, club, theatre&bar.Offersgluten-freeoptionsandwheelchairaccess.

Paperino’sWestEnd (L) 227ByresRoad, Glasgow, G128UD., Foodserved: Mon–Sunnoon–10.45pm. Capacity: 180.Paperino’sthreebranchesinGlasgow, allservingtraditionalItaliancuisine, be-ganin1991withtherestaurantonSauchiehallStreet. Thewhite-washedwallsandterracottatilesonthefloorisadecorativethemethattheownersrepeatedwhentheyopenedtheByresRoadbranchin2005. Bigger, brighterandshinier,thenewerrestauranthasacontemporaryatmosphere. A goodselectionofap-petisersincludesbruschettas, antipastoandplentyofvegetarianoptions, suchasstuffedmushroomsandmozzarellasticks.

LaParmigiana (H,V) 447GreatWestern Road, Glasgow, G128HH., Food served:Mon–Satnoon–2.30pm, 5.30–10.30pm. ClosedSun. Capacity: 50.LaParmigianaisaproper, old-schoolItaliandiningexperience, withgracious,knowledgeable–ifslightlysolemn–Italianwaitersinlongstarchedaprons, amenuthatshowcasesaccomplishedItaliancooking, andawinelistthatwouldnotlookoutofplaceinarespectedrestaurantinRome. Andafter30yearsontheGlasgowsceneithasjustregaineditstwoAA rosettes. Deep, richredwalls, crisplinen, angledwoodentablesandhushedtonesallconspiretocreateaserious,grown-upfoodieexperience.

StravaiginCaféBar (B,V) 28GibsonStreet, Glasgow, G128NX,Foodserved: Mon–Fri10am–10.30pm; Sat/Sun11am–10.30pm. Capacity: 85.A WestEndinstitution, StravaiginCaféBaroffersallthefashionableandlocallysourcedeatingofthemainrestaurantdownstairsinthebasement, butinamorerelaxedsetting, andaspopularwithfamiliesasitislocalpopstars. Gluten-freeoptionsandwheelchairaccessavailable; outdoortablesforsmokers.

Ubiquitous Chip (H) 12 Ashton Lane, Glasgow, G12 8SJ., Food served: Mon–Satnoon–2.30pm, 5.30–11pm; Sun12.30–3pm, 6.30–11pm. Capacity: 130.Therestaurantconsistsofaglass-roofed, cobbledcourtyard liberally suppliedwithleafyplantsandasmallfishpond, givingitapleasantoutdoor/indoorfeel.Theserviceisslick, professionalandwarm. Theever-changingmenuisexcit-ingtoreadletalonesample, withtheemphasisoninventivedishesusingfreshingredients. Theimpressivewinelistwillleaveyoustrugglingtochoose.

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LaVallée Blanche (H) 360Byres Road, Glasgow, G12 8AY., Food served: Tue–Frinoon–2.15pm, 5.30–10.30pm; Satnoon–11.30pm; Sunnoon–10.30pm. ClosedMon.Capacity: 76.LaValléeBlanchesucceedsinshowingsensitivitytoshrinkingbudgetswithoutcompromisingontaste. Justasitsnameandcosychaletinspireddécorimply,the‘WhiteValley’turnsoutthesortoftraditionalFrenchfoodyoucoulddevourafteradayinthemountains. Themenuchangesthroughouttheyeartofavourseasonallocalproduce.

TheWeeCurryShop (B) 23AshtonLane, Glasgow, G128SJ,Foodserved: Mon–Thunoon–2.30pm, 5.30–10.30pm; Fri/Satnoon–11pm; Sun5.30–10.30pm. Capacity: 31.Ifchainrestaurantsare theanathematogoodeating, thenitsgoodtosee theMotherIndiastablecontinuingtodefyreceivedwisdomwiththeirgrowinglineofWeeCurryShops. TherearebranchesalsoinByresRoadandatCowcaddens.

Usefulnumbers, andemergencyinformation

GlasgowTaxis(hackneycabs)01414297070. LocalTaxiRanks: Hillheadsub-waystationandoppositeBotanicalGardens (GreatWesternRoad/ByresRoadintersection).

PrivateHire: WestEndRadioCars01419547070, CanniesburnTaxis01419563333, GlasgowAirportTaxis01418886363.

PublicTransport TravelineScotland http://www.travelinescotland.com/welcome.do, 08712002233(chargesvary).

StrathclydePartnershipforTransport(SPT) http://www.spt.co.uk/

FirstbusGlasgow http://www.firstgroup.com/ukbus/scotland/swscot/home/

Scotrail http://www.scotrail.co.uk/, 08457484950(NationalRailEnquiries).

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Ses

sion

s Monday12th, 1545–1730Bute P01: GalaxyFormationandEvolutionintheLow-RedshiftUniverse

WithMulti-WavelengthSpectroscopicSurveysG255 P02: MassiveStars: NewViewsoftheirFormationandProgenyG226 P03: 10YearsofCluster: thePast, PresentandFutureofMulti-point

MeasurementsofSpacePlasmasFore P04: NewViewsofSolarActiveRegionsfromHinodeandSTEREO

G466 P05: STFC CurrentFacilities

Tuesday13th, 1045–1230G255 P06: ScienceontheWaytoSKA -Session1Bute P07: FirstresultsfromtheHerschelSpaceObservatoryG226 P08: MagnetosphericphysicsofJovian-typeplanetsandUltra-cool

dwarfsFore P09: UKSP /MIST MissionsForum: theStateoftheArtandFuture:

OpportunitiesG466 P10: SoftwareAstronomy: HowtoDoAstronomybyLookingThrough

aComputer

Tuesday13th, 1545–1730Bute P11: TheDarkArtofDarkMatter-Session1G466 P12: WaterintheSolarSystemandBeyondG226 P13: MagnetospheresandIonospheresThroughouttheUniverseFore P14: MagneticCouplingoftheSolarAtmosphere:

Magneto-SeismologyoftheSolarAtmosphereG255 P15: VISTA:PerformanceandSurveys

Wednesday14th, 1045–1230Bute P16: ScienceontheWaytoSKA -Session2G466 P17: A NewErainAstrochemicalStarFormationG226 P18: GeneralMIST ScienceSession1Fore P19: EnergeticParticlesintheSolarSystemandAstrophysical

Plasmas: ObservationsandTheoryG255 P20: ExplosionsintheDistantUniverse-Session1

Wednesday14th, 1545–1730Bute P21: TheDarkArtofDarkMatter-Session2G466 P22: DisksandStarsatExtremelyHighAngularResolutionFore P23: MagneticReconnection

G226 P24: SolarInfluencesintheHeliosphereG255 P25: ExplosionsintheDistantUniverse-Session2

Thursday15th, 1045–1230Bute P26: TheSloanDigitalSkySurvey: theLegacyandFutureG466 P27: StellarPopulationsinGalaxiesG226 P28: GeneralMIST ScienceSession2Fore P29: ModellingofDynamicSolarPlasmas

G255 P30: PulsarAstrophysics

Friday16th, 1045–1230Bute P31: TheRoleofFeedbackinGalaxyEvolutionG226 P32: StellarandExoplanetaryMagnetismG466 P33: PublicEngagementinAstronomy, SolarandSolarSystemPhysicsFore P34: UKSP GeneralSession

G255 P35: NewTechnologiesforFutureInstruments, TelescopesandMissions

P01 GalaxyFormationandEvolutionintheLow-RedshiftUniverseWithMulti-WavelengthSpectroscopicSurveys[2010April12, 15:45, p43]

WecannowstudythelowredshiftUniverse(z<0.5)usingextensivepopulationstatisticswithverylargegalaxynumbersandhighredshiftcompletenesslevels.Inthissession, welookforwardtocontributionsonnewgalaxysurveyanalyses,whichmakeextensiveuseofmulti-wavelengthdatasetsbycombininginforma-tion fromSDSS,GALEX,Herschel, UKIDSS,etc., onhighlights from thenewGAMA survey, andonresultsfromthemostrecentgalaxyformationmodels.

The"GalaxyAndMassAssembly"(GAMA) surveyisamajorredshiftsurveyforgalaxyformationwithanalreadyuniquespectralenergydistributioncoverage:GALEX-UV,SDSS-optical, UKIRT-NIR,Herschel-FIR andGMRT-radio. GAMAhasmeasuredsince2008over90knewspectraover 150sq.deg., probinginasystematicandcomprehensivemannerthefaintgalaxypopulationoveratimes-panoffourbillionyears(z<0.5).

A NAM sessionfocussedaroundGAMA scienceandsimilarmulti-wavelengthopportunitiesinthelowredshiftUniverseisideallytimedwiththefirstGAMAdatareleaseplannedformid-2010. ThemajorsciencegoalscoveredbyGAMAcomprisemulti-wavelengthgalaxygroupstudies, theevolutionofthebaryoniccontentoftheUniverseandtheefficiencywithwhichgalaxiesformasfunctionofenvironment.

Organisedby: PederNorberg(IfA,UniversityofEdinburgh), IvanBaldry(Liver-poolJohnMooresUniversity)15:45 AaronRobotham: GalaxyAndMassAssembly(GAMA):Thenextgen-

erationsurveyofsurveys.16:05 DavidHill: GAMA photometryandtheCosmicSpectralEnergyDistri-

bution16:20 AlfredoCarpineti: Thecolours, AGN properties, environmentsandstar

formationhistoriesofbulgedominatedpost-mergersinthelocaluni-verse

16:40 CristinaC.Popescu: Modelling theUV/optical FIR/submmemissionfromSpiralGalaxies

17:00 ClaireBurke: ScaleSizeEvolutionofBrightestGalaxies17:15 PosteradvertsPosters LeonidasChristodoulou: GalaxyClusteringUsing Photometric Red-

shiftsEmmaCurtisLake: StudyinggalaxyevolutionwithFMOS (FibreMulti-ObjectSpectrograph)IgnacioFerreras: A newapproachtodisentanglingstarformationhis-toriesfromsurveydataJenniferGupta: A new sampleof "blazars" to study the relationshipbetweenradio-loudAGN andgalaxyformationEdoIbar: Theradiospectralindexofsub-millimetregalaxies.RussellJohnston: RobustmethodstoprobesourceevolutioningalaxyredshiftsurveysLeeKelvin: GAMA:SingleandMulti-ComponentGalaxyModellingErinMacdonald: TheALFALFA HI AbsorptionSurveyMatthewPrescott: RedandBlueSatelliteGalaxiesintheGalaxyandMassAssemblySurveyAwatRahimi: AbundancegradientsinsimulatedgalaxydiscsDmitrijSemionov: ModellingradiationfieldsingalaxiesusinganewradiationtransfercodeBoonKokTan: NGC 2976&NGC 3351: 12CO(3-2)ObservationsanditsCorrelationwithPAH 8um

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P02 MassiveStars: NewViewsoftheirFormationandProgeny[2010April12, 15:45, p45]

Massivestars, despitetheirrarity, playadisproportionateroleingalaxiessincetheydominatetheirionizingbudget, chemicalenrichmentandfeedback. Thissessionwillfocusupontopicalquestionsrelatingtothepropertiesandevolutionofhighmassstars(mass-loss; significanceofLuminousBlueVariablestage; bi-narystatistics)andtheirprogeny(core-collapseSN;magnetars; GRBs)andwouldinvolve latest results fromTarantula surveyESO largeprogramme, PanSTARRsetc.

Theadventofnewinstruments(SCUBA-2), satellites(Herschel)andprogressinfindingtheearlieststagesofmassivestarformation(egtheIR darkclouds)-aswellastherecentrenewedinterestinmodelsofhowmassivestarsform-alsomakeittimelytoholdasessiondedicatedtotheformationofmassivestars. InthissessionweaimtodrawtogetheralltheexcitingworkbeingdoneintheUK inthisfield, whichwealsohopewillactasacatalysttodrivefuturecollaborationsintheUK communityforALMA projects.

Organisedby: PaulCrowther(UniversityofSheffield), StuartLumsden(Univer-sityofLeeds)15:45 AdamAvison: ProbingSitesofMassiveStarFormation: TheMethanol

MultiBeamSurvey16:05 Heather Cooper: The RMS Survey: Near Infra-Red Spectroscopy of

MassiveYoungStellarObjectsInTheNorthernHemisphere16:25 BenDavies: A MassiveStarisBorn: thecircumstellardisk, envelope,

andbi-polaroutflowofW33A16:40 ChristopherEvans: TheVLT-FLAMES TarantulaSurvey17:00 MatthewAustin: Anultravioletstudyofthetheweakwindproblemin

O stars17:15 AndrewMason: High-MassX-rayBinariesintheNIR:Orbitalsolutions

oftwohighlyobscuredsystems.Posters JaneBuckle: A wide-field, high-resolutionviewofNGC2264

SimonClark: MultiplegenerationsofmassivestarformationinclustercomplexesStaceyHabergham: Type Ibc supernovae indisturbedgalaxies: evi-denceforatop-heavyIMFMarkRushton: TheevolutionofthepeculiarvariableV838Monocero-tis2002-2009

P03 10YearsofCluster: thePast, PresentandFutureofMulti-pointMeasurementsofSpacePlasmas [2010April12, 15:45, p46]

In2010, ESA'sClustermissionwillhavebeenorbitingtheEarthfor10yearsmak-ingmeasurementsofthemagnetosphere, bowshockandsolarwind. Duringthistime, Clusterhashelpedtoimproveourunderstandingofvariousaspectsofso-larterrestrialandplasmaphysicsincludingmagnetosphere-ionospherecoupling,wavesandcurrentsinthemagnetosphere, reconnectionandfluxtransport, andplasmashocks. Inthecomingyears, Clusterwillbeabletomakethefirstmulti-pointinvestigationsofauroralaccelerationprocesses. Withproposalsfornewmulti-spacecraftmissionsunderconsideration, andwithClusterhavingreachedthismilestone, itistimelytoreviewthese10yearsworthofobservationsandcon-siderhowtheseobservationscanhelpusinpreparingforfuturemulti-spacecraftmissionssuchasCross-ScaleandMMS.

Organisedby: ColinForsyth(UniversityCollege, London, MSSL),AndrewWalsh(UniversityCollege, London, MSSL),AndrewFazakerley(UniversityCollege, Lon-don, MSSL),ElizabethLucek(ImperialCollege, London), MattTaylor(EuropeanSpaceAgency)

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15:45 C.PhilippeEscoubet: 10Years of Cluster: HighlightsofMulti-pointMeasurementsinSpacePlasmas

16:15 KhuromKiyani: UsingCluster’sobservationsofthesolarwindtoinves-tigatecollisionlessplasmaturbulence--currentresultsandoutlookforthefuture

16:30 AndrewWalsh: TheMagnetotailPlasmaSheetRevisited: ClusterPEACEStatistics

16:45 JonathanEastwood: Averagepropertiesofthemagneticreconnectioniondiffusion region in theEarth’smagnetotail: 2001–2005Clusterobservationsandcomparisonwithsimulations

17:00 RogerDuthie: DoBBF eventscontributetoinnermagnetospheredipo-larisation? A threeyearstatisticalstudyusingconcurrentClusterandDoubleStarobservation

17:15 ColinForsyth: Multi-spacecraftobservationsofauroralelectronaccel-erationbyCluster

Posters MikeHapgood: ExtendingCluster JSOC scienceoperationsover thepasttenyears

MattTaylor: Here, thereandeverywhere: gettingafeelforboundarylayerevolutionusingmultipointmeasurements

P04 NewViewsofSolarActiveRegionsfromHinodeandSTEREO [2010April12, 15:45, p48]

Sincetheirlaunchin2006, theHinodeandSTEREO spacecraftshaveprovideduswithnewinsightsintothephysicsofsolaractiveregions. ThecombinationofthreetelescopesaboardHinodeisofferingunprecedentedcoveragefromopticaltoX-raystherebyenablingstudiesofthecouplingbetweendifferentlayersofthesolaratmosphere. Using theobservationsrecordedby theExtreme-ultravioletImagingSpectrometer(EIS) aboardHinodewehavemeasuredphysicalplasmaparameterssuchaselectrondensity, temperatureandflowsinactiveregionsasawhole, aswellas in individualcoronalstructures. TheEUV ImageraboardSTEREO has provideduswith true 3-dimensional topologyof active regions.ThenewobservationalresultsobtainedbyHinodeandSTEREO haveprovideduswithsomeveryimportantconstraintsonthetheoreticalmodellingofactiveregionloops. Inordertoexplainthenewobservationstherehavebeensignificantadvancesinthemodellingofactiveregionloops. Therefore, itisworthwhileandtimelythatwecompareourtheoreticalmodelswithobservationalresults.

Organisedby: AlisonWallace(UniversityCollege, London, MSSL),HelenMason(DAMTP,Cambridge), GiuliodelZanna(DAMTP,Cambridge)

15:45 AlanHood: Whatcantheorydoforyou?

16:00 GiulioDelZanna: Hinode/EIS observationsofactiveregionloops

16:15 LenCulhane: PlasmaMotionsandMagneticReconnectionHeatinginthe2007, May19Flare

16:30 DurgeshTripathi: Activeregionmoss: basicphysicalplasmaparame-tersandtheirtimevariability

16:45 SarahMatthews: Coronalsignaturesofasunspotlight-bridge

17:00 LucieGreen: WhatcanHinodeobservations tellusabouteruptionsfromsigmoidalactiveregions?

17:15 Posteradverts

Posters CarolineAlexander: X-rayBright PointTopology StudywithHinodeandSTEREO

DavidGraham: ObservationsofflareribbondensitiesusingHinode/EIS

IainHannah: Regularized inversion techniques for recoveringDEMsfromHinode/XRT data

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RobertO'Neil: Relationshipbetweenmagneticfieldandcoronalout-flowsinactiveregions

SantiagoVargasDominguez: Convectiveplasmaaroundsolarpores

P05 STFC CurrentFacilities [2010April12, 15:45, p49]

ThissessionwillprovideacommunityforumtodiscussthecurrentstatusofUKastronomicalfacilities, includingVLT,Gemini, HerschelandSCUBA2. Thefocuswillbeonscienceresultsandfutureprospects, andcurrentandfuturedevelop-mentsininstrumentation.

Organisedby: DerekWard-Thompson(CardiffUniversity)

15:45 RaySharples: UpdateontheKMOS SpectrographforESO VLT

16:00 DimitraRigopoulou: HerschelandSPICA:pushingthefrontiersintothecoolcosmos

16:15 SimonGarrington: e-MERLIN

16:30 JohnRicher: ALMA:statusreportandfirstscience

16:45 GaryDavis: JCMT andUKIRT:GoodNewsandBadNews

17:00 DavidNutter: EarlyresultsfromSCUBA2

17:15 DavidClements: WhitherUK-LedGround-BasedSubmmAstronomy?

Posters RobertBarnsley: FRODOSpec: RoboticSpectroscopyusingtheLiver-poolTelescope

JoaoBento: A studyoftheSuperWASP detectormaps

NeilMawson: TheLiverpoolTelescope: ObservationswiththeSTILT(SmallTelescopesInstalledatLT) widefieldinstruments

P06 ScienceontheWaytoSKA -Session1 [2010April13,10:45, p50]

BothEuropeanandUK visiondocumentsplaceSKA alongsideE-ELT asthekeyground-basedfacilitiesforfutureastronomy. Newradiotelescopesonthepath-waytotheSKA arenowstartingtocomeonlinewithfirstscienceresultsimmi-nentfromeMERLIN,eVLA andLOFAR.Intheseparallelsessionswewillshow-casetheseresultsalongsidethosefrommorematureinstrumentsliketheGMRT(e.g jointGMRT/Herschel surveys). Plans for involvement of theUK sciencecommunityinSKA anditsprecursors(ASKAP andMeerKAT) willbeoutlined.

Organisedby: MattJarvis(UniversityofHertfordshire)

10:45 SteveRawlings: PathwaytotheSKA

11:10 JohnMcKean: EarlyresultsfromthecommissioningofLOFAR

11:25 AlanPenny: A SETI pilotprogrammewithLOFAR

11:40 MattJarvis: TheMeerKAT DeepContinuumSurvey

12:00 PrinaPatel: RadioWeakGravitationalLensingwithVLA andMERLIN

P07 FirstresultsfromtheHerschelSpaceObservatory [2010April13, 10:45, p50]

HerschelwaslaunchedinMay2009andstartedtakingsciencedatainOctober2009. ThefirstscientificresultsfromthismissionwillbeavailableintimeforNAM,allowingtheUK astronomicalcommunityafirstlookatsciencefromthismajorUK andEuropeanmission. Thetimelinessofthissessionislikelytoleadtopressandpublicinterest.

Organisedby: DaveClements(ImperialCollege, London)

10:45 MattGriffin: Herschel: statusandin-orbitperformance

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11:00 AnthonySmith: InitialresultsfromHerMES:theHerschelMulti-tieredExtragalacticSurvey

11:15 EmmaRigby: TheHerschel-ATLAS:A firstlook

11:30 MatthewSmith: TheHerschelVirgoClusterSurvey(HeViCS)

11:45 DerekWard-Thompson: EarlyHerschelResultsonStarFormation

12:00 NeilPhillips: FirstresultsfromtheDEBRIS survey

12:15 RogerWesson: SPIRE FTS spectraofthreecarbon-richevolvedobjects

Posters HarsitPatel: SWIRE 70micronselectedGalaxies: FollowupandLumi-nosityFunction

P08 MagnetosphericphysicsofJovian-typeplanetsandUltra-cooldwarfs [2010April13, 10:45, p51]

Currentevidencesuggests thatultracooldwarfsbridgethegapbetweensolar-typestarsthatexhibitcoronalactivityandjovian-typeplanetspossessinglarge-scalemagnetospheresandneutralatmospheres. Evidenceforthisplanet-likebe-haviorhasbeenobservedintheradioregime, whereultracooldwarfshavebeenfoundtoproduceperiodicpulsesofextremelybright100%circularlypolarizedradioemission. Thegasgiantsofthesolarsystem–particularlyJupiterandSaturn–havebeenthesubjectofmuchintensiveresearchwithinthelastdecade. SpacemissionssuchasGalileoandCassinihavegivenusunprecedentedinsightintothephysicalprocesseswhichshapethemagneticfields, plasmapopulationsandauroraeoftheseplanets. It is thusanexcellentopportunityforNAM tobringtogethertheultracoolstarcommunityandtheplanetarycommunityandtohigh-lighttheexcellentresearchbeingdoneinmagnetosphericphysicsbeyondtheEarth.

Organisedby: GerryDoyle(ArmaghObservatory), NickAchilleos(UniversityCollegeLondon)

10:45 ChrisArridge: Giantplanetmagnetospheres: JupiterandSaturn

11:10 GreggHallinan: Dynamicspectraofindividualradiopulsesinanul-tracooldwarf

11:30 DavidSouthwood: Sourceofperiodicradioemission; lessonsfromSat-urn

11:45 AlexeyKuznetsov: Numericalsimulationoftheelectron-cyclotronmaserinstabilityinthemagnetospheresofbrowndwarfs

11:55 JonathanNichols: VariationofSaturn'sUV aurorawithSKR phase

12:10 StuartLittlefair: UltraspecObservationsofTVLM 513-46546

12:20 PaulineLang: ThePeculiarbehaviourofRadioEmissioninFullyCon-vectiveStars

Posters RobertKing: PhysicalParametersofUltracoolDwarfs: TheYoungandTheOld

AdamMasters: Structure anddynamics of the boundary of Saturn'smagnetosphere

JaphethYates: Influenceofupstreamsolarwindconditionsonatmo-sphericflowsatJupiter

ShenghuaYu: Mapping radioemitting-regionon low-mass starsandbrowndwarfs

P09 UKSP /MIST MissionsForum: theStateoftheArtandFuture: Opportunities [2010April13, 10:45, p52]

Thissessionwillbesplitintotwoparts: TheStateoftheArtwillreviewthecurrentstatusofUK involvementinupcomingmissions; FutureOpportunitieswillbeanopencommunitydiscussiononfuturemissionsandopportunitiesbeyondand

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outsidethecurrentCosmicVisionsprogramme. Thestatusofcurrentmissionsandfacilitieswillbepresentedinanaccompanyingpostersession. Thisisyourchancetovoiceyouropiniononwherewemovenextinscienceatacrucialtime!"

Organisedby: DavidWilliams(UniversityCollege, London, MSSL),ColinForsyth(UniversityCollege, London, MSSL),LouiseHarra(UniversityCollege, London,MSSL)

10:45 RobertWalsh: NASA SDO,itsscienceandtheUCLandata-hub

11:00 RichardMarsden: SolarOrbiter: exploring theSunandHeliosphereconnection

11:15 MicheleDougherty: EuropaJupiterSystemMission

11:30 MikeHapgood: Scienceopportunitiesforgeospacestudies?

Posters DanielleBewsher: Determinationofthephotometriccalibrationandlarge-scaleflatfieldoftheSTEREO HeliosphericImagers: I.HI-1

ChrisCarr: TheRosettaPlasmaConsortium

AndrzejFludra: SOHO CoronalDiagnosticSpectrometer

RichardHarrison: TheSTEREO Mission

MarkLester: SuperDARN UK:A newresource tostudyof theupperatmosphere

ElizabethLucek: ClusterFGM:currentandfuturescientificopportuni-ties

ChristopherOwen: SolarOrbiter: TheSolarWindAnalyserInvestiga-tion

JianSun: HinodeUnveilsA NewSun

P10 SoftwareAstronomy: HowtoDoAstronomybyLookingThroughaComputer [2010April13, 10:45, p54]

Increasingly, astronomyishappeninginsoftware. Thisisn'tjustthereductionoftelescopedata(theoldStarlink/IRAF world, wherethesoftwarewasjustanaspectofobservationalastronomy), butastronomywherethecomputeristheprimaryinstrumentdeliveringthescience. Thiscoverssimulationsanddatamining, butmostrecentlyalsovarioustypesoffundamentallyonlineapproachestohandingtheever-intensifyingdatadeluge, includingvirtualobservatory, crowdsourcing,socialastronomy, andthesemanticweb.

Inthisspecialsessionwewillbringtogetherleadersinthevariousstrandsofsoft-wareastronomy. TheUK hasaleadingroleinthis(arguably)newsubdiscipline,andthisspecialsessionwillbuildthiscommunity, andcementitslinkstothemore... traditionalroutesfromphotonstoelectrons.

Organisedby: NormanGray(UniversityofGlasgow)

10:45 IntroductoryRemarks

11:00 DuncanForgan: NativeSyntheticImagingofSmoothedParticleHydro-dynamicsSimulations

11:20 AnnaMariaMassone: SoftwaretoolsforprocessingRHESSI visibilities

11:40 ChrisLintott: SupportingDistributedScience: RunningGalaxyZoo

12:00 MarkJones: Developingskillsfor“softwareastronomy”: aninnovativedistancelearningprojectforOpenUniversitystudents

12:20 AvonHuxor: GraphicInterfacestoExplanatoryAnalysisofAstronomi-calImageDatabases

Posters RobBlake: TheWFCAM ScienceArchive

JohnBrooke: DataIntegrationinHeliophysics

OliverButters: TheSuperWASP publicarchive

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TobiaCarozzi: VOeventstriggeredbygravitywaves

NigelHambly: NewinfraredandopticalimagesservicesintheVO

MarkHolliman: VirtualObservatoryServicesatWFAU

BonnieSteves: ThehierarchicalstabilityofexoplanetarysystemsofBi-narystarsusingtheCaledonianSymmetricFour-Bodymodelwithanewglobalregularisationalgorithmtohandlecloseencounters

P11 TheDarkArtofDarkMatter-Session1 [2010April13,15:45, p56]

Thegoalofthissessionistounderstandthemysteriousdarkmatterthatcom-prises95%ofthemattercontentoftheUniverse. TheUK isattheforefrontofresearchinthefieldsofCosmologyandParticlePhysicswithstrengthsinboththeoryandobservations. Wewelcomeanyresearcherintheoryorobservation,fromallfields, workingtowardsthegoalofunderstandingdarkmatter. Togetherinthissessionwewilldiscusskeyquestionssuchas: “howcanwebetterexploitsynergiesbetweendirectandindirectdetection?”Toaiddiscussion, inadditiontothetwoscheduledparallelsessionstherewillbea20-30personbreak-outsession, tobeheldonthemorningof14thApril. Ouraimistofosteracollabo-rativeenvironmentatthemeetingthatwillleadtostrongUK-ledresearchinthisrapidlydevelopingfield.

Organisedby: CatherineHeymans(IfA,UniversityofEdinburgh), RichardMassey(IfA,UniversityofEdinburgh), TomKitching(IfA,UniversityofEdinburgh)

15:45 PawelMajewski: Directdetectionofdarkmatter

16:10 JustinRead: DarkMatterintheMilkyWay

16:35 JorgePenarrubia: The impactofdarkmattercuspsandcoreson thesatellitegalaxypopulatio

16:50 AlinaKiessling: ApplicationsofaNewandRapidSimulationsMethodforWeakLensingAnalysis

17:00 EdwardThomson: Wave-mechanicsofLargeScaleStructure

17:10 JakobJonsson: WeighinggalaxiesusinggravitationallylensedSNLS su-pernovae

17:25 Posteradverts

Posters ChrisBrook: Dodarkmatterhaloshavecusps?

OlafDavis: Extremevaluestatistics: predicting the frequencyof thedensestclustersandsparsestvoids

MartinFeix: TeVeS andthestraightarcofA2390

IgnacioFerreras: Probingthedarkmatterhalosofearly-typegalaxiesvialensing

HodaGhodsi: SuddenFutureSingularitymodelsasanalternativetoDarkEnergy?

GülayGürkan: Thenewpathtotimedelays?

VictoriaHamilton-Morris: LoCuSS:WeakLensingAnalysisof21GalaxyClustersatz=0.15-0.3

CatherineHeymans: Probing theDarkUniversewithWeakLensingTomographyandtheCFHTLS

DanielJohn: A NewPixonWeakLensingClusterMassReconstructionMethod

CraigLawrie: Theimpactofdelensinggravitationalwavestandardsirensondeterminingcosmologicalparameters

HongshengZhao: BrightIdeasandDarkThoughts: "UniversalBaryonicScale"at"MaximumHaloGravity"

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P12 WaterintheSolarSystemandBeyond [2010April13,15:45, p57]

Thissessionaimstocutacrosssomeofthetraditionalsubjectareasinastrobiol-ogy, bringingpeopletogethertoconsidertheorigin, distributionandactionofwaterinthegalaxy. TopicscoveredwillspantherangefromwaterintheSolarSystem–i.e. theMoon, Marsandasteroids, andicybodies(e.g. comets, Europa)–toexoplanetaryatmospheres.

Organisedby: MonicaGrady(OpenUniversity)

15:45 PedroLacerda: TheDensitiesofKuiperBeltObjects

16:00 HenryHsieh: TheMain-BeltComets: Long-livedIceintheInnerSolarSystem

16:15 JayFarihi: TheFrequencyandCompositionofWater-RichExtrasolarAsteroids

16:30 IngoWaldmann: Characterisationofexoplanetaryatmospheres

16:45 DavidKipping: NightsidePollutionofExoplanetTransitDepths

17:00 MikakoMatsuura: ObservationsandmodellingofwatervapourlinesintheHerschelSPIRE FTS spectrumoftheluminousred-supergiant, VYCanisMajoris

17:15 AnitaRichards: AmasingWater

P13 MagnetospheresandIonospheresThroughouttheUniverse[2010April13, 15:45, p58]

MagnetospheresareubiquitousthroughouttheUniverse, beingfoundininter-stellargasclouds, intheenvironmentsofblackholesandotherdegenerateob-jectsaswellasaroundplanetsandstars. Galactic, heliospheric, andexoplane-tarymagnetospheresaddyetanotherdimensiontothisimmensevariety. Iono-spheresandionospheric-likecollisionalplasmaenvironmentsarealsoubiqui-tous in planetary environements andmuch of the collisional plasma physicsfoundinplanetaryionospherescanalsobeappliedtoastrophysicalsystemssuchasaccretiondiscs. Thesolarsystemcontainsadiversearrayoffascinatingplan-etarymagnetospheresandionospheres, eachuniquebutsharingthesamefun-damentalphysicalprocesses. Solar systemenvironmentshavebeenexploredusingavarietyof techniquesandsuch investigationshavebenefited fromtheuniqueadvantageofbeingabletoincludein-situmeasurements. Thishasledtoasignificantbodyofunderstandingonspaceplasmaswhichishighlyapplicabletoastrophysicalsystems. Comparativestudiesbetweenplanets(includingEarth)andmoonsthroughoutthesolarsystemallowinvestigationsofawiderangeofphysicalconditions, suchasmagneticfieldconfigurationandcompositionoftheplasma. Comparisonsbetweenplanetaryandastrophysicalenvironmentsrevealinterestingsimilaritiesinsystem-levelbehaviour, suchasphaseshiftsanddriftingperiodsinperiodicplanetaryradioemissionsandtheintermittentbehaviourofsomepulsars.

We invite contributions that discuss the physical processes and structures inastrophysicalandplanetarymagnetospheres, ionospheresandionospheric-likecollisionalastrophysicalplasmaenvironments. Weanticipatepapersthatstudygeneralmagnetosphericandionosphericphysicsleadingtoauniversalunder-standingofmagnetospheresandionospheresandwhichexploretheapplicabilityofcollisionalionosphericplasmaphysicstoastrophysicalplasmaenvironments,suchasaccretiondiscs.

Organisedby: ChrisArridge(UniversityCollege, London, MSSL),BenStappers(UniversityofManchester), AlanWood(AberystwythUniversity), AndyBreen(AberystwythUniversity)

15:45 Introductoryremarks

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15:50 SteveMiller: TheroleofH3+inplanetaryatmospheres

16:10 PatrickWeltevrede: Radioobservationsofhighlyenergeticpulsars

16:30 ThomasNeukirch: Simplemodelsforclosedfieldlineregionsofthree-dimensionalrigidlyrotatingmagnetospheres

16:45 NicholasAchilleos: TheInfluenceofHotPlasmaPressureonMagne-tosphericStructureatSaturn

17:00 EuanBennet: AlfvénWavesinPartially-IonisedandRecombiningPlas-mas

17:15 RobertKidd: Searching forEvidenceofStarSpots inSTEREO Helio-sphericImagerData

Posters GeraintJones: TheShockingSizeofCometMcNaught

KevinRonald: LaboratoryExperimentstoinvestigatethemechanismsofAuroralKilometricRadiation

AlanWood: IonlosstotheSolarWindfromVenusatSolarMinimum

P14 MagneticCouplingoftheSolarAtmosphere:Magneto-SeismologyoftheSolarAtmosphere [2010April13, 15:45, p60]

Highresolutionobservations(TRACE,HINODE,STEREO) arerevolutionizingourviewsandunderstandingofphysicalprocessesinthesolaratmosphereandtheconnectivitybetweenvarious regionsandphenomena takingplace in theso-laratmosphere. Combiningobservablepropertiesofwavesandoscillationsinvariousmagneticstructureswiththeoretical(includingnumerical)modelling, al-lowusdeterminationof notonlymagnitudeofmagneticfieldsbut also sub-resolutionstructuringusingseismologicaltechniques. Thesessionaimstoreviewrecentadvancesinthefieldofmagneto-seismologyandputindividualdynami-cal/energeticphenomenaintoamuchwiderglobalpicture.

Organisedby: I.Ballai(UniversityofSheffield), R.vonFaySeibenburgen(Uni-versityofSheffield), M.Mathioudakis(Queen'sUniversityBelfast)

15:45 GaryVerth: Magnetoseismologyof thechromospherewith torsionalAlfvénwaves

16:00 DavidJess: ThelinkbetweenSodiumintensityenhancementsandthephotosphericmagneticfield

16:15 TomVanDoorsselaere: Anatomyofaslowwaveinacoronalloop

16:25 SergeiZharkov: Evidenceofmagneto-acousticwavesinphotosphericobservationsofasunspot

16:35 MikeMarsh: ExploitingtheCoronalSlowMode

16:45 RichardMorton: Properties ofMHD waves in plasmawith variablebackground

16:55 DavidPascoe: CoupledAlfvénandKinkOscillationsinCoronalLoops

17:05 PhilipCrockett: BigBrightPoint, SmallBrightPoint, Cardboardbox

17:15 DavidRobertson: Theeffectofdensitystratificationonthetransverseoscillationsoftwoparallelcoronalloops

Posters IstvanBallai: TRACE/EUV observationofdrivenlooposcillations

NickyChorley: Longperiodoscillationsinsunspots

HughHudson: Flaresandglobalwaves, includingseismic

MarialejandraLuna: Longitudinaloscillationsinanexpandinghotcoro-nalloop.

BeniaminOrza: PhasemixingintheSolarCorona

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P15 VISTA:PerformanceandSurveys [2010April13, 15:45,p61]

VISTA'sfirstScienceruns(10daysofScienceVerification)completedon02-NovandVISTA wasacceptedbyESO inmidNovember. ‘DryRun'surveys(100hrforeachofthesixsurveys)started03-NovandtheVISTA PublicSurveysformallybeginon15-Feb2010.

Whilstitwillbealittleearlytoexpectmuchnewscience, thepurposeofthissessionwillbetoprovideatimelyreportontheperformanceandcapabilitiesoftheas-builtVISTA,andontheprogressandresultssofarfromthefirstdataoftheESO publicsurveyswithVISTA.

Organisedby: JimEmerson(QueenMary, UniversityofLondon)

15:45 JimEmerson: VISTA Performance

15:55 JamesLewis: TheVISTA sciencepipeline

16:05 JamesDunlop: UltraVISTA

16:20 MattJarvis: TheVISTA DeepExtragalacticObservations(VIDEO) Sur-vey

16:35 WillSutherland: VIKING,theVISTA Kilo-degreeInfraredGalaxySurvey

16:50 JosephFindlay: HighredshiftquasarsintheVIKING field.

17:00 RichardMcMahon: TheVISTA HemisphereSurvey

17:15 Maria-RosaCioni: TheVMC survey-I.StrategyandEarlyScienceData

Posters GemmaBagheri: A near-infraredstudyoftheMagellanicSystemwithVISTA.

RossCollins: TheVISTA ScienceArchive

NicholasCross: FindingvariablesusingtheVISTA ScienceArchive

RoaldGuandalini: FirstobservationsofstellarclustersintheLMC fromtheVMC survey

PhilipLucas: VISTA VariablesintheViaLactea(VVV) andnewUKIDSSGPS highamplitudeIR variables

Maria IdaMoretti: Variable Stars in theVISTA near-infraredY, J, KssurveyoftheMagellanicCloudSystem(VMC)

P16 ScienceontheWaytoSKA -Session2 [2010April14,10:45, p62]

BothEuropeanandUK visiondocumentsplaceSKA alongsideE-ELT asthekeyground-basedfacilitiesforfutureastronomy. Newradiotelescopesonthepath-waytotheSKA arenowstartingtocomeonlinewithfirstscienceresultsimmi-nentfromeMERLIN,eVLA andLOFAR.Intheseparallelsessionswewillshow-casetheseresultsalongsidethosefrommorematureinstrumentsliketheGMRT(e.g jointGMRT/Herschel surveys). Plans for involvement of theUK sciencecommunityinSKA anditsprecursors(ASKAP andMeerKAT) willbeoutlined.

Organisedby: MattJarvis(UniversityofHertfordshire)

10:45 TomMuxlow: Thee-MERGE LegacySurvey

11:05 EmmaRigby: Theluminosity-dependenthigh-redshiftcut-offofthera-dioluminosityfunction

11:25 AndyLawrence: OriginoftheCosmicRadioBackground

11:45 HansikKim: Thespatialdistributionofcoldgasinhierarchicalgalaxyformationmodels

12:00 RogerDeane: HighResolutionRadioObservationsofIRAS FSC10214

Posters JoannaBulger: TheOVRO OphiuchusPre-Stellar (OOPS) Survey: A3.4mmContinuumEmissionStudyofCircumstellarMaterial

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P17 A NewErainAstrochemicalStarFormation [2010April14,10:45, p63]

Thissessionwillprovideanoverviewofcurrentresearchinastrochemistry, bring-ing together thefieldsofobservationalastronomy, theoreticalmodelling, andlaboratoryastrochemistry. TheemphasiswillbeonastrochemicalresearchinareasthatwillreapthebenefitsofcurrentandplannedmissionssuchasJCMT,Herschel, ALMA andJWST,particularlyareasassociatedwithstarformationinboththenearandfaruniverse.

Thisisanexcitingtimeforthestudyofastrochemicalprocessesinthefaruni-verse. Detectionsofwaterice, amorphousandaromatichydrocarbonsatred-shifts 2, anddetectionsintheearlyuniverse(e.g. CO atz 6)areprovidingthestimulus for research into star formation inhigh redshift galaxies, whereverydifferentphysicalparametersareneeded formodels. In thenearbyuniverse,theimprovedspatialandspectralresolutionofferedbynewinstrumentationwillstronglyinfluencemodelsofstarandplanetformation, enabling, evenenforcing,theinclusionofdynamicsinchemicalmodelsof, forexample, nearbycircum-stellardisks. Suchmodelsandobservationsalsorequireinteractionwithdevel-opinglaboratorystudies. Ournewviewofthemolecularcomplexityinthelocalgalaxywillchangedramaticallytheunderstandingofformationprocessesandevolutionarystages.

Organisedby: JaneBuckle(CavendishAstrophysics, Cambridge)

10:45 StevenCharnley: IsotopicFractionationinPrimitiveMaterial: Quanti-fyingtheContributionofInterstellarChemistry.

11:00 EstelleBayet: Extragalactic star formationactivity -propertiesof theverydensegas

11:15 MartinMcCoustra: Photon- and Electron-drivenProcesses inModelInterstellarIces

11:30 GaryFuller: AstrochemistryintheALMA era

11:45 NatalieChristopher: FirstResultsfromSHINING -SurveywithHerscheloftheISM inNearbyINfraredGalaxies

12:00 VictoriaFrankland: TowardsUnderstandingtheFormationofWaterintheInterstellarMedium

12:15 ZainabAwad: Thedeuteriumchemistryinlowandhighmassstarform-ingregions

Posters AliAbdulgalil: LaboratoryStudiesofNon-thermalDesorptionofAce-tonitrilefromIcyGrainMantles

SeanChapman: InvestigatingtheOnsetofSilicateCrystallizationintheEarlyStagesofStarFormation

HelenChristie: ChemistryofdenseclumpsnearmovingHerbig-Haroobjects

KerryHebden: ChemicalevolutioninNGC 6302(theButterflynebula)

NadyaKunawicz: Hotcoremodelsatlowmetallicity

PaulRuffle: TheXgearProject -A NewEra forAstrochemicalMod-elling?

P18 GeneralMIST ScienceSession1 [2010April14, 10:45, p65]

Magnetospheric-Ionospheric-Solar-Terrestrial(MIST) researchconcernsphysicalprocesseswithintheSun-Earthsystem, othersolarsystembodiesandexo-planets;inparticularthesolar/stellarwind, moonsandplanetaryatmospheresandmag-netospheres. TheMIST generalsessionisdesignedtoaddressthoseaspectsof

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currentMIST researchnotexplicitlycoveredinothersessions, suchasneutralat-mospherescience, ULF wavesandwave-particleinteractions, auroralandiono-sphericelectrodynamics, andground-basedstudiesofthecoupledmagnetosphere-ionosphere system. All researcherswhoare interested inanyaspectofMISTsciencearethereforeinvitedtotakepart.

Organisedby: AdrianGrocott(UniversityofLeicester), EmmaWoodfield(Uni-versityofLancaster), AndrewFazakerley(UniversityCollege, London, MSSL)

10:45 MarkLester: CoordinatedgroundandspaceobservationsofGeospace:A viewfromtheground

11:05 JamesHutchinson: ObservationsofGeomagneticStormsoveraSolarCycle: SomeInitialFindings

11:20 AlanWood: Comparisonsofplasmatransportinthehigh-latitudeiono-spheresoftheEarthandVenus.

11:35 CathrynMitchell: GPS Plasmsphericimaging

11:55 Katie Turnbull: ModellingGeomagnetically InducedCurrents in theNationalGridusingSAMNET.

12:10 MartinFullekrug: SpritesandRelativisticElectronBeamsAboveThun-derclouds

12:25 Posteradverts

Posters EwanDawson: EstimatingtheExtremesinGeomagneticActivityAcrossEurope

TimothySpain: MagneticfieldparallelcurrentsintheUCL-CTIP model

JimWild: Presentdaychallenges inunderstanding thegeomagnetichazardtonationalpowergrids

P19 EnergeticParticlesintheSolarSystemandAstrophysicalPlasmas: ObservationsandTheory [2010April14, 10:45,p68]

Thegenerationofahigh-energynon-thermalparticlepopulationisaprominentfeatureofmanymagneticactivityprocesses insolar systemandastrophysicalplasmas. Examples includeauroralparticleacceleration inplanetarymagne-tospheres, solarand stellarflaresandenergeticprocesses incompactobjectssuchaswhitedwarfs, neutronstarsandblackholes. Thissessionaimstofur-therourunderstandingof thephysicalprocessesunderlying thegenerationofhigh-energynon-thermalparticlepopulations indifferentphysical regimesbygivingresearchersfromdifferentareastheopportunitytopresenttheirworkandexchangetheirideas. Weencouragethesubmissionofpapersonboththetheo-reticalandobservationalaspects, includingtheaccelerationprocess, thepropa-gationandtransportofenergeticparticlesfromthelocationofacceleration, andtheirdetection.

Organisedby: ThomasNeukirch(UniversityofStAndrews), SilviaDalla(Uni-versityofCentralLancashire)

10:45 PhilippaBrowning: ParticleaccelerationattheSun

11:05 AndrewWright: AuroralParticleAccelerationattheEarth

11:25 ChristinaBurge: ParticleAccelerationinthePresenceofWeakTurbu-lenceatanX-TypeNeutralPoint

11:38 MykolaGordovskyy: Particleaccelerationinafragmentingcurrentsheet

11:51 Rim Turkmani: Electrons re-acceleration at the chromospheric foot-pointsofSolarFlares

12:04 HamishReid: SolarFlareAcceleratedElectronTransport through theTurbulentDensityoftheSolarWind

12:17 MichelePiana: Fromelectronmapstoaccelerationmechanismsofen-ergeticparticlesintheflaringSun

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Posters MarinaBattaglia: ImagingobservationsofX-rayalbedoinacompactdiskflareNicolasBian: ParallelelectricfieldgenerationbyAlfvénwaveturbu-lenceSilviaDalla: RoleoflatitudeofsourceregioninsolarenergeticparticleeventsEwanDickson: MeasurementofAnisotropyinSolarFlareElectronSpec-trausingRHESSI HardX-RaySpectroscopy.KeithGrady: ParticleMotion and EnergyGains in KinematicMHDmodelsofCollapsingMagneticTrapsJingnanGuo: Temporal, Spectral, andSpatialAnalysesofX-rayEmis-sionComponentsinImpulsiveSolarFlaresIainHannah: CantheinfluenceofturbulentdensityperturbationsinthecoronabedetectedinflareX-rayspectrum?ChuanLi: Coronalmagnetic topologyandthesolarsourceofmajorSEP eventsSiming Liu: Stochastic ParticleAcceleration by CompressiveModeswithIncompressiveModeInducedSpatialDiffusionHeatherRatcliffe: Electromagneticemissionfrombeam-generatedLang-muirwavesDavid Speirs: Numerical simulation ofmagnetospheric electron cy-clotronemissionCraigStark: MagnetosphericParallelElectricFields

P20 ExplosionsintheDistantUniverse-Session1 [2010April14, 10:45, p70]

Explosiveextragalactictransientsarenowbeingroutinelydiscoveredacrosstheelectromagneticspectrumcomplementedbydatafromincreasinglysensitivegrav-itationalwaveandneutrinoobservatories. Thecombinationof such facilitiesopensupnewopportunitiesforthestudyoftransientphenomenaincludingGamma-RayBursts, Supernovaeandtidaldisruptionbysuper-massiveblackholes. Weproposeapairof sessionsatNAM2010 todiscusscurrent results in this fast-movingareaandtoencouragecoordinatedresearchcombiningphotonicandnon-photonicdata.

Theproposedsessionshavetwomaingoals: (1)todiscussthemostinterestingrecentdiscoveriesintheexplosiveUniversefromworkingfacilities; and(2)toenhancediscussionandinteractionbetweenthesediversecommunitiesanden-couragenewworkingrelationships. Thesessiontopicswouldbeapproximatelydividedinto:

• Supernovae: newdiscoveriesanddiversityofexplosionphysics;

• GRBs: recenthighlightsandpotentialforthefuture;

• Thepotentialof futuresurveysand facilities forcharacterisingexplosivetransients.

Wewouldparticularlyencourage reports fromthecurrent / futureuseof sur-veysandfacilitiesinvolvingUK partners(e.g. Swift, Fermi, Pan-STARRS,LOFAR,LIGO,MAXI,HESS,CTA).

Organisedby: PaulO'Brien(LeicesterUniversity), StephenSmartt(QueensUni-versityBelfast), JonathanGranot(UniversityofHertfordshire), NialTanvir (Le-icesterUniversity)10:45 MarkSullivan: LuminoustransientsinthedistantuniversewithPTF and

SNLS

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11:30 MorganFraser: Identifyingandchacterising theprogenitorsof core-collapsesupernovae

11:45 JoanneBibby: SurveyoftypeIb/csupernovaprogenitorsinnearbystar-forminggalaxies.

12:00 ZachCano: TheGRB-SN connection: ExploringGRB progenitorswithmulti-wavelengthobservations

12:15 ValeriuPredoi: Searchforgravitational-waveinspiralsignalsassociatedwithshortGamma-RayBurstsduringLIGO'sfifthandVirgo'sfirstsci-encerun

P21 TheDarkArtofDarkMatter-Session2 [2010April14,15:45, p71]

Thegoalofthissessionistounderstandthemysteriousdarkmatterthatcom-prises95%ofthemattercontentoftheUniverse. TheUK isattheforefrontofresearchinthefieldsofCosmologyandParticlePhysicswithstrengthsinboththeoryandobservations. Wewelcomeanyresearcherintheoryorobservation,fromallfields, workingtowardsthegoalofunderstandingdarkmatter. Togetherinthissessionwewilldiscusskeyquestionssuchas: “howcanwebetterexploitsynergiesbetweendirectandindirectdetection?”Toaiddiscussion, inadditiontothetwoscheduledparallelsessionstherewillbea20-30personbreak-outsession, tobeheldonthemorningof14thApril. Ouraimistofosteracollabo-rativeenvironmentatthemeetingthatwillleadtostrongUK-ledresearchinthisrapidlydevelopingfield.

Organisedby: TomKitching(IfA,UniversityofEdinburgh), RichardMassey(IfA,UniversityofEdinburgh), CatherineHeymans(IfA,UniversityofEdinburgh)15:45 Reviewofthismorning'sbreak-outsession15:55 DavidMiller: UsingtheLHC toprobeDarkMatterinphysicsbeyond

theStandardModel16:20 MarkusHorn: TheZEPLIN-III DarkMatterSearchExperiment16:35 FergusSimpson: UnmodifiedGravity16:50 MatthewWalker: EmpiricalConstraintsontheDarkMatterContentof

DwarfSpheroidalGalaxies17:05 CarlosFrenk: Cosmologyonsmallscales: thestructureof(mostly)dark

matterhalos

P22 DisksandStarsatExtremelyHighAngularResolution[2010April14, 15:45, p72]

ThissessionaimstohighlighttotheUK astronomycommunityrecentresultsandprogressinthefieldofopticalandinfraredlong-baselineinterferometry. Opti-calinterferometrycanpresentlyachieveangularresolutionsashighasverylongbaselineinterferometry(VLBI) andcancombineuptosixtelescopes. Imagingofdisksandstarsatextremelyhighangularresolutioncanbeachievedwiththeexistinginterferometricfacilities. Weinvitecontributionswhichdiscusscurrentresults, encouragecollaborativeresearchandexploitationoftheexistinginstru-ments.

Organisedby: EttorePedretti(UniversityofStAndrews)15:45 ReneOudmaijer: Opticalandnear-infraredinterferometryofstarsand

disks16:10 MyriamBenisty: ThecomplexinnerdisksofHerbigAeBestars16:23 JennyPatience: Investigatingtheinnerdisksofyoungstars16:36 FabienBaron: ImagingwithMIRC attheCHARA interferometer16:49 RachelSmith: Resolvingdebrisdiscsinterrestrialplanetregionswith

MIDI-VLTI

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17:02 JohnYoung: CharacterisingtheconvectionpatternonBetelgeuse

17:15 Foteini(Claire)Lykou: Dustydiscsaroundevolvedstars

Posters DavidBuscher: ScienceProspectswiththeMagdalenaRidgeObserva-toryInterferometer(MROI)

JamesGordon: ImagingshockfrontsinMiravariables

EttorePedretti: Mappingstar-spotsontheRS CVnbinary ζ And

AlexRea: TheMagdalenaRidgeInterferometerFringeTracker

AnitaRichards: Dosingleoldstarsejectclumps?

P23 MagneticReconnection [2010April14, 15:45, p73]

Magneticreconnectionisafundamentalprocessinastrophysical, solarandmag-netosphericplasmas. Previouslymagneticreconnectionwasunderstoodintermsof two-dimensionalMHD modelswhichsometimes leadtooversimplistican-swersregardingthedynamicsandenergeticsoftheprocess. Nowadaysthree-dimensionalfluidmodels(MHD,Hallormulti-fluid)orkineticmodelsarethestateoftheartandthesemodelsproduceamorecomplexanddiverserangeofreconnectionphenomena. Whilethisnewgenerationofmodelsprovidesmuchmorerealisticanswers, whichcanbebettercomparedwithobservations, theyarealsomorechallengingtounderstand. Weinvitecontributionsfromastrophysics,solarandmagnetosphericphysicsforajointsessionontheoryandobservationsofmagneticreconnection, aprocesswhichiskeytoourunderstandingofplasmadynamics.

Organisedby: GunnarHornig(UniversityofDundee)

15:45 MichaelBareford: A NanoflareDistributionGeneratedbyRepeatedRelaxationsTriggeredbyKinkInstability

16:00 AlisonWallace: Doesmagnetichelicityeffectactiveregionevolutionandenergetics?

16:15 DavidPontin: Regimesofmagneticreconnectionat3D nullpoints

16:30 PeterWyper: 3D MagneticNullpoints: LocalisedFantiltingandTor-sionalReconnection

16:45 Robert Fear: Comparisonofmodels of flux transfer event formationusingpredictedandobservedasymmetry

17:00 AntoniaWilmot-Smith: Relaxationofbraidedcoronalloopsbymultiplesmall-scalereconnectionevents

17:15 ClareParnell: 3-D Magneticreconnectionatseparators

Posters GunnarHornig: Turbulentrelaxationofbraidedmagneticfields

EhsanPedram: A surveyofHXR emissionofseismicallyactiveandquietX-classwhite-lightflares

FionaWilson: PropertiesoftheDistributionFunctionofaVlasov-MaxwellEquilibriumfortheForce-FreeHarrisSheet

P24 SolarInfluencesintheHeliosphere [2010April14, 15:45,p75]

ThissessionwilladdressourcurrentunderstandingoftheinfluenceoftheSunonthesurroundingheliosphericenvironment, andtheopportunitiesforfutureresearchinthisarea. Conventionally, wehaveconductedremotesensingofthenear-Sunenvironmentandhaveperformedinsitumeasurementsfurtheroutintheheliosphere; thishasledtotwodistinctareasoffocus. Howeverinrecentyears, andparticularlywiththeadventoftheSTEREO mission, manynewdataanalysistechniqueshavebeendevelopedthatbridgethisdividebetweenstudiesofthenear-Sunandinterplanetaryspaceenvironments.

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ThereisstillmuchtolearnaboutthelinksbetweentheSunandtheheliosphere,inparticulartheoriginsoftheambientsolarwindandsolarejecta, theirstructureandevolutionastheypropagateintointerplanetaryspaceandtheirsubsequentinteractionswithplanetsandothersolarsystembodies. Thissessionwilldrawtogetherourcurrentknowledgeofthephysicswithinthesolar-heliosphericen-vironment, whilstaddressingthemethodologiesrequiredtofurtherunderstandandprogressthisareaofscience, withparticularemphasisontheexploitationofmultiplemissions.

AllresearcherswhoareinterestedintheSun-heliosphereconnectionareinvitedtoparticipateandtocontributetothissession.

Organisedby: KimberleySteed(UniversityCollege, London, MSSL),JackieDavies(RutherfordAppletonLaboratory), RichardHarrison(RutherfordAppletonLab-oratory), ChrisDavies(RutherfordAppletonLaboratory)

15:45 Introductoryremarks

15:50 MathewOwens: Probing the evolution of coronal andheliosphericstructureswithsuprathermalelectrons

16:15 AnthonyYeates: Non-potentialenhancementoftheSun'sopenmag-neticflux

16:30 PeterGallagher: PropagationofanEarth-DirectedCoronalMassEjec-tionin3D

16:45 MarekKukula: SolarStormwatch: acrowd-sourcingapproachtoun-derstandingCoronalMassEjections

17:00 SrividyaSubramanian: Small scale transient featuresatcoronalholeboundaries: apossiblesourcefortheslowsolarwind?

17:15 LidiavanDriel-Gesztelyi: Are there imprintsofhotplasmaoutflowsfromactiveregionsinthesolarwind?

Posters RobertBentley: TheHeliophysicsIntegratedObservatory

MarioBisi: A ComprehensiveStudyofthe13-15May2005SolarEvent(s)

ChristopherDavis: AssessingtheaccuracyofCME speedandtrajectoryestimatesfromSTEREO observationsthroughacomparisonofindepen-dentmethods

KimberleySteed: Investigatingtheobservationalsignaturesofmagneticcloudsub-structure

AnthonyWilliams: CharacterisingtheSTEREOHeliosphericImagersig-naturesofCorotatingInteractionRegions

P25 ExplosionsintheDistantUniverse-Session2 [2010April14, 15:45, p76]

Explosiveextragalactictransientsarenowbeingroutinelydiscoveredacrosstheelectromagneticspectrumcomplementedbydatafromincreasinglysensitivegrav-itationalwaveandneutrinoobservatories. Thecombinationof such facilitiesopensupnewopportunitiesforthestudyoftransientphenomenaincludingGamma-RayBursts, Supernovaeandtidaldisruptionbysuper-massiveblackholes. Weproposeapairof sessionsatNAM2010 todiscusscurrent results in this fast-movingareaandtoencouragecoordinatedresearchcombiningphotonicandnon-photonicdata.

Theproposedsessionshavetwomaingoals: (1)todiscussthemostinterestingrecentdiscoveriesintheexplosiveUniversefromworkingfacilities; and(2)toenhancediscussionandinteractionbetweenthesediversecommunitiesanden-couragenewworkingrelationships. Thesessiontopicswouldbeapproximatelydividedinto:

• Supernovae: newdiscoveriesanddiversityofexplosionphysics;

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• GRBs: recenthighlightsandpotentialforthefuture;

• Thepotentialof futuresurveysand facilities forcharacterisingexplosivetransients.

Wewouldparticularlyencourage reports fromthecurrent / futureuseof sur-veysandfacilitiesinvolvingUK partners(e.g. Swift, Fermi, Pan-STARRS,LOFAR,LIGO,MAXI,HESS,CTA).

Organisedby: PaulO'Brien(LeicesterUniversity), StephenSmartt(QueensUni-versityBelfast), JonathanGranot(UniversityofHertfordshire), NialTanvir (Le-icesterUniversity)

15:45 JonathanGranot: Highlights fromFermiobservationsofGamma-RayBursts

16:30 MassimilianoDePasquale: GRB090510, thefirstcasestudyofashortGRB withGeV extendedemissiondetectedbyFermiandSwift.

16:45 AntoniaRowlinson: DiscoveryoftheafterglowandhostgalaxyofthelowredshiftshortGRB 080905A

17:00 RachelTunnicliffe: InvestigationoftheenvironmentofshortgammarayburstGRB090510withaviewtoconstrainingtheprojenitor.

17:15 TomMuxlow: Discoveryofanunusualnewradiosourceinthestar-forminggalaxyM82: Faintsupernova, supermassiveblackhole, oranextra-galacticmicroquasar?

Posters LauraWatson: FindingtheSourceofUHECRsusingBayesianAnalysisofPierreAugerData

P26 TheSloanDigitalSkySurvey: theLegacyandFuture [2010April15, 10:45, p76]

TheSloanDigitalSkySurvey (SDSS) is themostproductive surveyof the sky(Madrid&Macchero2009), withover65 thousandcitations to theSDSS viaADS.Inthissession, wewillgiveanoverviewoftheoutstandingSDSS discover-iessincefirstlightadecadeago, whilealsolookingforwardtothenewSDSS-III(www.sdss3.org)projectwhichcontinuesthislegacy. Thesessionwillcoveradiverserangeofscience(planetstodarkenergy)andtopics(dataaccesstopub-licationissues).

Organisedby: BobNichol(ICG,Portsmouth)

10:45 IvanBaldry: Globalpopulationstatistics, bimodalityandmultivariatedistributionsofgalaxieswithSDSS.

11:03 NicholasRoss: TheSDSS-III BaryonOscillationSpectroscopicSurvey(BOSS):FirstResults

11:21 MathewSmith: SDSS-II SNe-AnOverviewandHostGalaxyProperties

11:39 JonLoveday: GalaxyClusteringintheSDSS

11:57 CristianoSabiu: Higher-OrderClusteringOfLuminousRedGalaxiesInTheSDSS

12:04 BorisGaensicke: Whitedwarfsastracersofstellar, binary, andplane-taryevolution

12:11 ZengHuaZhang: Discoveryof thefirstwideL dwarf+giantbinarysystemandeightotherultra-cooldwarfsinwidebinaries

12:18 AshleyRoss: AnalysingtheClusteringofPhotometricallySelectedGalax-ies

12:25 AvonHuxor: EvidenceofTidalStrippingofthreecompactelliptical(cE)galaxiesdiscoveredinSDSS DR7

Posters DavidMurphy: DVORACDetector-TheDurhamVOronoiRed-sequenceAutomatedClusterDetectorfornext-generationpanoramicsurveys

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LiekevanSpaandonk: BinarypopulationsinSDSS:A newdiagnosticforsystemparametersofevolvedwhitedwarfbinaries

P27 StellarPopulationsinGalaxies [2010April15, 10:45, p78]

Thestudyofstellarpopulationsprovidesvitalcluesontheevolutionofgalaxiesandtheunderlyingphysicalprocesses. Theinterpretationofphotometricandspectroscopicdatafromresolvedandunresolvedstellarsystemsrestsontheac-curacyofstellarevolutionmodelsandmodelatmospheres, theircombinationintopopulationsynthesismodels, andthetechniquesemployedtofittheorytoobservations.

Thegoalofthissessionistodiscussourcurrentknowledgeofresolvedandunre-solvedstellarpopulations, focusingonboththedifferencesamongmodelsandmethodsweemploy inouranalyses, and thedevelopmentsnecessary for thefullexploitationofdatafromthecurrent-andnext-generationofastronomicalfacilities.

Organisedby: MaurizioSalaris(LiverpoolJohnMooresUniversity)

10:45 RussellSmith: Learningaboutstellarpopulationsinunresolvedgalaxies

11:05 SusanPercival: Systematicuncertaintiesinherentinstellarpopulationsynthesismodelsandtheirimpactonintegratedspectraofstellarpop-ulations: A modeller'sperspective.

11:20 JohnEldridge: BPASS:BinaryPopulationandSpectralSynthesis

11:35 SugataKaviraj: Theroleofminormergersinthestarformationhistoryofearly-typegalaxies

11:50 IgnacioFerreras: ConstrainingtheInitialMassFunction

12:05 MichaelBarker: TheLastMajorEpochofDiskGrowthinM3312:20 Posteradverts

Posters RichardHutcheon: KinematicbiasinexoplanetsurveysOliviaJones: Crystallinesilicatesaroundoxygen-richAsymptoticGiantBranchStarsintheLargeMagellanicCloud

LisetteSibbons: TheAGB populationand themetallicitygradient inNGC 6822

BejaminTatton: AGB StarsinWLMPaulWoods: ThestellarpopulationsintheLargeMagellanicCloud

P28 GeneralMIST ScienceSession2 [2010April15, 10:45, p79]

Magnetospheric-Ionospheric-Solar-Terrestrial(MIST) researchconcernsphysicalprocesseswithintheSun-Earthsystem, othersolarsystembodiesandexo-planets;inparticularthesolar/stellarwind, moonsandplanetaryatmospheresandmag-netospheres. TheMIST generalsessionisdesignedtoaddressthoseaspectsofcurrentMIST researchnotexplicitlycoveredinothersessions, suchasneutralat-mospherescience, ULF wavesandwave-particleinteractions, auroralandiono-sphericelectrodynamics, andground-basedstudiesofthecoupledmagnetosphere-ionosphere system. All researcherswhoare interested inanyaspectofMISTsciencearethereforeinvitedtotakepart.

Organisedby: AdrianGrocott(UniversityofLeicester), EmmaWoodfield(Uni-versityofLancaster), AndrewFazakerley(UniversityCollege, London, MSSL)

10:45 TimothySpain: SCANDI:All-skyviewofmeso-scalespatialstructureinthethermosphereandion-neutralcouplingoverSvalbard

11:05 AndrewSenior: ObservationsandmodellingofartificialD-regionheat-ingseenbyARIES

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11:20 HannahVickers: Observationsofdouble-peakedHF radarspectraduetomixedechoesfromnaturalandartificialplasmairregularities

11:35 SheilaKanani: Overviewof lowenergyelectronobservations in thevicinityofSaturn'smoonEnceladus

11:50 GabbyProvan: Evidencefortheoccurrenceof 10.6hmagneticfieldoscillationsinSaturn’sequatorialmagnetosphere

12:05 DavidAndrews: Magnetospheric-periodoscillationsinSaturn'sequa-torialmagnetosphereandopentaillobesthroughouttheCassinimis-sion

12:20 PosteradvertsPosters Ciaran Beggan: Interpolation of external magnetic fields over large

sparsearraysusingSphericalElementaryCurrentSystemsEllenClarke: AnestimationoftheCarringtonflaremagnitudefromsolarflareeffects(sfe)inthegeomagneticrecordsAdrianGrocott: SuperDARN observationsofthesub-auroralconvec-tionresponsetoenhancedgeomagneticactivityJohnHargreaves: ThedriftofauroralradioabsorptionpatchesobservedbyimagingriometerStephanieKellett: NatureoftheringcurrentinSaturn’sdaysidemagne-tosphereGemmaKelly: TowardsmodellingofhighlatitudemagneticfieldsfromsatellitedataAnthonyWilliams: TrackingsolarwindstructuresfromtheSunthroughtotheorbitofMarsEmmaWoodfield: CombiningincoherentscatterradardataandIRI2007tomonitortheopen-closedfieldlineboundaryduringsubstorms.

P29 ModellingofDynamicSolarPlasmas [2010April15, 10:45,p79]

Newspacemissionswiththeirhigherspatial, spectral, andinparticulartemporalresolutionareprovidingapictureofamoredynamicsolaratmosphere. Suchobservationsrequireatime-dependentmodellingapproach. Whatisthestatusofcurrentmodellingasregardstransientionization? Wheredowestandregardinghydrodynamicandmagneto-hydrodynamicmodellingoftheconstantlychangingsolaratmosphereonsmallscales? Thissessionwillbelargelydirectedtowardsthemodellingofvariousdynamic featureswhetherobservedfromthegroundorspacebasedinstruments. ItwillbringtogethernotonlyMHD andHD expertsbutitwillalsodiscussvariousaspectsofthepresentmodellingrelatingtoatomicphysics.

Organisedby: GerryDoyle(ArmaghObservatory), MariaMadjarska(ArmaghObservatory)10:45 MariaMadjarska: PlasmapropertiesofanX-rayjetfrommulti-instrument

co-observations: SUMER/SoHO,EIS/XRT/HinodeandEUVI/SECCHI/STEREOA andB

11:00 PeterCargill: A newenthalpy-basedapproachtothetransitionregioninanimpulsively-heatedcorona

11:15 JiaoyangDing: Chromosphericmagnetic reconnection: implicationsforjet-likeeventsandcoronalheating

11:30 DavidTsiklauri: TheHydrodynamicEvolutionofImpulsivelyHeatedCoronalLoops: ExplicitAnalyticalApproximations

11:45 KarenMeyer: Non-LinearForce-FreeModeloftheSolarMagneticCar-pet

12:00 UrmilaMitraKraev: Detailedobservationsandmodellingofasmallflare

33

12:15 HughPotts: Theopticaldepthofwhite-lightflarecontinuumPosters ZhenghuaHuang: Observationand3D modellingofacoronalbright

pointGuiyunLiang: CalculationandapplicationofR-matrixelectron-impactexcitationdataforionsofinteresttoastrophysicaldiagnosticmodellingProchetaMallik: AlfvénIonisationintheSolarPhotosphereSrividyaSubramanian: Whatblinkersactuallyare?KamalamVanninathan: SpiculesandCoronalHeatingLidiavanDriel-Gesztelyi: MagneticreconnectionalongQSLs-amajordriverofactiveregionoutflows

P30 PulsarAstrophysics [2010April15, 10:45, p81]

More than40yearsafter theirdiscovery, pulsars (and latterly, magnetars) stillpresentextraordinarychallengestoastrophysicalmodellinganddataanalysis.Progressisbeingmadeinunderstandingtheunderlyingphysicsthatgovernstheemissioncharacteristicsof theseextraordinaryobjects, butmuch remainsun-clearorunknown. Thephysicsoftheinterior, thecrustandtheatmosphereofneutronstarsrequireustoconfrontourunderstandingofthebehaviourofmat-terandradiationinextremeconditions. Thereisawealthofobservationaldata,andadiversityofapplicationforthisdata, thatmakesaclearercomprehensionofemissionprocessesandimplicationsallthemoreurgent. Weinvitesubmis-sionsfromallthoseinterestedpartieswhoareaddressingthefollowingtopicsintheirresearch: neutronstarinteriors; neutronstarcrusts; neutronstaratmo-spheres; pulsarplasmasandradiationmechanisms; behaviourofmatterunderextrememagneticandgravitationalfields; ultra-energeticprocessesinthepulsarenvironment; physicalinterpretationofradiationcharacteristicsofpulsarsandmagnetars.

Organisedby: NilsAndersson(UniversityofSouthampton), DeclanDiver(Uni-versityofGlasgow), AntoniodaCosta(InstitutoSuperiorTecnico-UTL,Lisbon)10:45 IntroductoryoverviewbyDonMelrose11:05 AntonioArmandodaCosta: PulsarElectrodynamics: TheRelativistic

KineticTheoryofRadiativePlasmas—TheGamma-raycut-off11:15 CristobalEspinoza: GlitchesintherotationofPulsars11:25 RobertFerdman: Testsofgeneralrelativityandbinaryevolutionstudies

usingpulsarobservations11:35 IkSiongHeng: A BayesianSearchForGravitationalWaveRing-downs

AssociatedWithPulsarGlitches11:45 WynnHo: CarbonatmosphereneutronstarinCassiopeiaA:Youngest

neutronstarintheGalaxy11:55 DominicKeogh: LatestHESS observationsofPulsarWindNebulae12:05 AndrewLevan: TheopticalandinfraredcounterpartofSGR 0501+451612:15 DeclanDiver: SurfaceextractionofelectronsinapulsarPosters EwanBarr: TheEffelsbergNorthernSkyPulsarSurvey

MatthewPitkin: KnownpulsarsascontinuousgravitationalwavesourcesSatoruSakai: TheeffectofGravitationalDistortionof SpacetimeonPulsarTimingNeilYoung: IntermittentRadioEmissionfromPSR B0823+26

P31 TheRoleofFeedbackinGalaxyEvolution [2010April16,10:45, p82]

Feedbackprocesses, bothfromsupernovaeandAGN,arebelievedtobeanim-portantprocessinshapingthegalaxyluminosityfunction, withdifferentmecha-

34

nismsbeingimportantatdifferentmassscales. Thissessionwilladdressfeedbackfrombothobservationalandtheoreticalperspectivesandinvestigatetheenerget-icsoftheprocessesatwork. MechanismsforthetriggeringandterminationofstarformationandAGN activitywillbeexplored.

Organisedby: ChrisSimpson(LiverpoolJohnMooresUniversity)10:45 SarahBryan: The impactof feedbackon theorbital contentofdark

matterhaloes.11:00 ElisaHouse: DiskHeating: ComparingtheMilkyWaywithCosmolog-

icalSimulations11:15 SamGeen: TheroleoffeedbackinMilkyWaysatellitegalaxyformation

usinghighresolutionsimulations11:30 GregStinson: StellarFeedbackinSPH GalaxyFormationSimulations11:45 MarkWestmoquette: Superstarclusterfeedbackfromlocaltogalaxy

scales12:00 JamesFalder: TheEnviromentsofAGN atz 112:15 AsaBluck: TheCo-EvolutionofMassiveGalaxiesandtheirSupermas-

siveBlackHolesoverthelast11.5GyrsPosters EmilyDown: Theorientationofaccretiondisksandjetsinquasars

KathrynHarris: ClusterandGalaxyEnvironmentsofQuasarsElizabethMannering: TheMulti-facetedX-rayactivityofthecomplete3CRR AGN sampleatz<0.1RachaelMcQuillin: MomentumdrivenfeedbackfromstellarnucleiKatePilkington: TheColdGasContentofBulgelessDiskGalaxiesCyprianRangel: SearchingforComptonThickAGN atz 2indeepX-rayfieldsXufenWu: StabilityandevolutionofclustergalaxiesinMOND

P32 StellarandExoplanetaryMagnetism [2010April16, 10:45,p84]

Thepastfewyearshaveseenthedetectionofmagneticstar-planetinteraction(SPI),anewlydiscoveredphenomenonthatmayyieldamethodofcharacteris-ingexoplanetarymagneticfieldsandconsequentlytheirinternalstructure. TheexistenceofmagneticSPI remainscontroversial, however, ifconfirmed, itwouldallowour Solar System tobeplaced in contextwith other planetary systemswithintheGalaxy. Asforstellarmagnetism, recentdiscoveriesincludethepos-sibledetectionofaremnantfossilfieldonahotmassivestar; thefirsteversurfacemapsofpre-mainsequencestarsintheclassicalT Tauriphaseoftheirevolution;thediscoveryofamagneticcycleonastarpossiblyinducedbyaknownorbit-ingclose-ingiantplanet; therapidincreaseinfieldcomplexityatthetransitionfromcompletelyconvectivelow-massstarstothosewithradiativecores; andthediscoveryofgloballystructuredmagneticfieldsontheintermediatemassHerbigAe-Bestars. Thissessionwillhighlight thelatestresults inthestudyofstellarmagnetismacrosstheHR diagram, andexoplanetarysystems.

Organisedby: ScottGregory(UniversityofExeter)10:45 GaiteeHussain: Stellarmagnetisminsolar-typestars11:15 RobJeffries: MagneticactivityinfastrotatingM-dwarfsaboveandbe-

lowthefullyconvectiveboundary11:30 StefanoBagnulo: StellarmagnetismthroughtheeyesoftheFORS1in-

strumentoftheESO VLT12:00 AlineVidotto: Theinfluenceofthestellarwindonclose-ingiantplanets12:15 GrantMiller: TheDopplerShadowofWASP-3bPosters RobertDeRosa: InvestigatingtheX-rayEmissionofA-typeStarsThrough

theMagneticActivityofUnresolvedLowerMassCompanions

35

ScottGregory: Testingtheabilityoffieldextrapolationmodelstopre-dicttheX-raypropertiesofpre-mainsequencestars

P33 PublicEngagementinAstronomy, SolarandSolarSystemPhysics [2010April16, 10:45, p85]

Overthepasttwoyears, publicengagementandoutreachinAstronomy, SolarandSolarTerrestrialPhysicsintheUK hasgainedmomentumduetotheInter-nationalHeliophysicalYear(IHY) andtheInternationalYearofAstronomy(IYA).

Inthissession, wewanttoexplorethenewopportunitiesthathavebeenopenedupbythesetwoprogrammes, hearingfromthepeoplewholedtheseinitiativesandotherswhoransuccessfulevents. SinceboththeIHY andIYA havenowfinished, it is timely todiscusswhathasbeensuccessfulaboutbothoutreachprogrammes, enablethoseinterestedinoutreachtodiscussbestpractice–andalsohow to retain themomentumand takeoutreach in theUK further. Thesessionwillcontainthefollowing:

• ReviewtalksfromanIHY andanIYA organisertosummarisethesuccessesoftheinternationalyears(20minseach);

• Contributedtalksfromthosewhoactivelyparticipatedinoutreachactivi-tiesduringIHY andIYA.Sharingofexperiencesandinsights;

• 'Speednetworking'–likespeeddating, butwiththeemphasisonnetwork-ingwithotherpeopleinterestedinoutreach;

• Discussion–generaldiscussion, howcanwesharebestpracticeacrossAstronomy, Solar&STP?HowdomaintainthemomentumforoutreachfromtheIHY andIYA?Howimportantinoutreachinthegrantsthatweapplyfor? Whatcountsasoutreachandwhatdoesn't?

Organisedby: DanHillier(ROE VisitorCentre), HelenMason(DAMTP,Cam-bridge), DanielleBewsher(UniversityofCentralLancashire)

10:45 Introductoryremarks

10:50 SteveOwens: BeyondIYA2009: SustainableScienceEngagement

11:00 LucieGreen: OutreachduringInternationalHeliophysicalYear

11:10 AlecMacKinnon: SchoolsoutreachfortheGlasgowNAM

11:15 IngeHeyer: IYA 2009ontheBigIslandofHawaii

11:20 OliviaJohnson: Beyondconstellationstories: communicatingcutting-edgescienceandengagingnewaudiencesthroughnovelplanetariumprogrammingfortheInternationalYearofAstronomy

11:25 HelenWalker: TheSocietyforPopularAstronomy'sTelescopesforSchoolsProject

11:30 DanHillier: UK DarkSkyDiscovery

11:35 CharlesBarclay: Astronomyinthecurriculum. DevelopmentsatKS4andKS5

11:40 AlisonWallace: Challenges of Public EngagementwithChildren inCare

11:45 HelenMason: Sun|trek-thefinalfrontier

11:50 JimWild: DidtheSunEarthPlanworkout?

11:55 DanielleBewsher: TheBigBang!

12:00 Discussion/soapbox

Posters MartinHendry: TheScottishSolarSystem

MartinHendry: DevelopmentofanAll-SkyCameraforOutreachAc-tivities

36

DonaldKurtz: SongsoftheStars: theRealMusicoftheSpheres

StuartLowe: 4YearsofPodcasting

RichardMorton: TheMusicoftheSunasaStar

P34 UKSP GeneralSession [2010April16, 10:45, p87]

Thissessionisdesignedtoaddressthecurrentsolarresearchnotcoveredinothersessions. Allresearcherswhoareinterestedinsolarphysicsareinvitedtotakepart.

Organisedby: DuncanMackay(UniversityofStAndrews), BarbaraBromage(UniversityofCentralLancashire), RekhaJain(UniversityofSheffield), EduardKontar(UniversityofGlasgow)

10:45 PaulHiggins: TheMagneticPropertiesofFlaringActiveRegions

11:00 NicolasLabrosse: NewsolarprominencediagnosticswithEIS/Hinode

11:15 JenniferHarris: Largeamplitudetransverseoscillationsinamulti-strandedEUV prominence, triggeredbytransientdisturbances

11:30 JamesMcLaughlin: Phasemixingofnon-linearAlfvénwaves

11:45 JamesThrelfall: Alfvénwavephase-mixinganddampingintheioncy-clotronrangeoffrequencies

12:00 FraserWatson: Automated detection and tracking ofmagnetic frag-mentsindecayingsolaractiveregions

12:15 DavidMacTaggart: Simulationsofmagneticfluxemergencewithanoverlyingfield

Posters VasilisArchontis: MagneticfluxemergenceandcoronaleruptionsintheSun

MarioBisi: Medium-andsmall-scaletransientsinthesolarwind

BarbaraBromage: AnomalousSolarCyclesandtheEvolutionofCoro-nalHoles

KenDere: ChiantiPy-A PythonInterfacetoCHIANTI

GarethDorrian: RapidOscillationsintheSolarAtmosphere

EduardKontar: HardX-RayStructureofLoopFootpointsinaSolarLimbFlare

XingLi: KineticAlfvénwavesandprotonvelocitydistributionin thesolarwind

BrendanO'Dwyer: SDO/AIA responsetocoronalhole, quietsun, ac-tiveregionandflareplasma

P35 NewTechnologiesforFutureInstruments, TelescopesandMissions [2010April16, 10:45, p89]

TheUK hasalongstandingheritageindevelopingthekeytechnologiesforsomeofthemostsuccessfulandstate-of-the-artinstruments, telescopesandmissionsforastronomy. Thenextgenerationofrequirementsposessomenewchallenges,and in thecurrentandnear-termeconomicclimate thecommunitywillmostlikelyhavetobemoreselectiveinidentifyingtheareaswhereourskillsarebestsuited. WhatarethenewtechnologiestheUK shouldbefocussinguponoverthenext10+years? Thesemayinclude, butarenotlimitedto, advanceddetec-torsandreadouts, novelnewlightweightsupportstructuresforspacetelescopes,portablehigh-coolingpower systems, highly reflectiveor transmissiveopticalcomponents, low-lossmaterialsforroomtemperatureandcryogenicoperation,newideasforactiveandadpativecontrolsystems, etc. Whilstmuchofthenear-tomid-termislikelytoconcentrateonE-ELT,SKA and2ndgenerationgravita-tionalwavetelescopeswemustalsonotlosetrackofmissionsthatarepotentially

37

furtherdownstream(e.g. spaceinterferometrysuchasFIRI andtheEinsteintele-scope). Thissessioninvitestalksandpostersfromastronomers, physicistsandengineers, withinbothacademiaandindustry, onanytechnologydevelopmentareasthatmightbenefitthemissionsofthefuture.

Organisedby: WayneHolland(UK ATC,Edinburgh), GilesHammond(Univer-sityofGlasgow), DaveMelotte(UK ATC,Edinburgh)

10:45 FraserClarke: HARMONI -A UK ledfirst light spectrograph for theE-ELT

11:00 SimonDoyle: LumpedElementKineticInductanceDetectorssuitableforlargearraysofastronomicaldetectors.

11:15 MelStrachan: Noveldeformablemirrordevelopmentsforastronomyapplications

11:30 StefanHild: High-PrecisionInterferometryandLow-LossmaterialsforfutureGravitationalWaveObservatories

11:45 IanHepburn: Milli-kelvincoolerfortheXMS instrumentontheInter-nationalX-rayObservatory

12:00 NicolaBeveridge: Hydroxidecatalysisbondingresearchforastronom-icalapplications

12:15 JanBergman: FIRST Explorer-spacebornelow-frequencyradioastron-omyusingpassiveformationflying

Posters JuliaKennedy: Reducingriskincryogenicinstrumentdesign: thermalconductivitymeasurementsattheCryogenicInstrumentationResearchLab

GiovannaTinetti: Probingtheatmospheresofextrasolarworldswithadedicatedmissionfromspace

RichardWhite: Astronomyatthehighestenergies: theCherenkovTele-scopeArray

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39

RA

SA

ftern

oon Session1: 14:00–15:20

WelcomefromRAS President, ProfessorAndyFabian.

Thefollowingmedalsandprizeswillbepresented. ThecitationsofmedalsandprizeswillbereadbyDrFionaSpeiritsandFraserWatson.

TheGoldMedalforGeophysics ProfessorJohnWoodhouseFRSUniversityofOxford

TheHerschelMedal ProfessorJamesHoughUniversityofHertfordshire

TheChapmanMedal ProfessorBernardRobertsUniversityofSt.Andrews

TheJackson-GwiltMedal DrCraigD MackayUniversityofCambridge

AwardForServiceToAstronomy ProfessorFranciscoSanchezInstituteofAstrophysicsoftheCanaryIslands

AwardForServiceToGeophysics DrFrankLowesUniversityofNewcastleuponTyne

GroupAchievementAwardForAstronomy SuperWASP teamrepresentedbyProfessorDonPollacco, Queen'sUniversity, Belfast

GroupAchievementAwardForGeophysics CHIANTI consortiumrepresentedbyProfessorKenDere, GeorgeMasonUniversity, Virginia

HonoraryFellowship ProfessorConnyAertsUniversityofLeuvenandRadboudUniversity, Nijmegen

HonoraryFellowship DrWlodekKofmanTheLaboratoryforPlanetology, Grenoble

TheFowlerAwardForAstronomy DrBarbaraErcolanoUniversityofCambridge

WintonCapitalAwardForAstronomy DrElizabethStanwayUniversityofBristol

WintonCapitalAwardForGeophysics DrDavidRobinsonUniversityofOxford

Thefollowingprizewinnerswereunabletoattend.

TheGoldMedalforAstronomy ProfessorDouglasGoughUniversityofCambridge

TheFowlerPrizeforGeophysics DrInekedeMoortelUniversityofStAndrews

ProfessorCarlosFrenkwillgivetheDarwin2010Lectureon‘Thestandardmodelofcosmogony: whatnext?’

Session2: 15:45–17:30

The futureofUK astronomy–adiscussionchairedbyProfessorAndyFabian(PresidentoftheAstronomyForum), includingpresentationsanddiscussionontheUK SpaceAgency, STFC andthe2011ComprehensiveSpendingReview. TheparticipantswillincluderepresentativesofSTFC andotheragencies.

41

Abs

tract

s LifeonTitanWilliamBains (RufusScientific/MIT)

Livingthingshavedistinctcharacteristicsthatconstraintheirpossiblechemistry, andhencewhereandhowwemightlookforthem. I willdiscusstheexampleofTitan: couldtherebelifeonthesurface? Majorlimitationsarethestability,solubilityandreactivityofthechemicalsthatmakeuplife, andenergysourcestodrivemetabolism. Iwillreviewhowtheseconstraintscanbeusedtoputlimitsonwherelifemightoccur, andthebiochemistrythatwemightlookforeitherremotelyorwhenwegetthere. ThesurfaceofTitandoesnotlookpromising, butifthereislifethereitwillbesimple, explosivelyunstableunderEarthconditions, and(tous)extremelysmelly.

TheSuperWASP ProjectAndrewCameron (UniversityofStAndrews)with

D. Pollacco, C. Hellier, R. West, and WASPConsortium

TheWASP consortiumiscurrentlytheworld'sleadingproducerofextra-solarplanetstransitingbrightstars. Itstwoautomatedwide-fieldcameraarrays, SuperWASP onLaPalmaandWASP-SouthatSutherland, eachimagesome15percentoftheskywithacadenceof7to8minutesforbetween4and8hourseachnight. Automatedsoftwareidentifiesstarsexhibitingtheone-percentdipsinlight, recurringeveryfewdays, thatbetraythepresenceofacompactsub- stellarcompanion.Efficientwinnowingoflikelycandidatesforradial-velocityfollowup, incollaborationwiththeGenevaandIAP/Haute-Provenceplanetsearchteams, hasledtothediscoveryofsome30transitingplanetstodate. InthispresentationI willannounceanumberofnewlyconfirmedWASPplanets. WASP'spublishedplanetdiscoveriesareenrichingourunderstandingoftheclosest-orbitinggasgiantplanetsaroundotherstars. Theyincludethehottest, mostinflatedandshortestperiodplanetsyetidentified. Manyhaverelativelymundanecircularorbitsinthestellarequatorialplane. Othershavehighlydisturbedeccentric,inclinedandevenretrogradeorbits. Theyrevealarichsetofplanetaryformationandmigrationhistories. Somearegrosslyinflatedbyacombinationofextremeirradiationandtidalenergydissipation. A smallnumberorbitsoclosetotheirstarsthattidalorbitdecaywillleadtotheirdestructionwithinthemain-sequencelifetimesoftheirhoststars. Aboveall, theWASP systemsarebright. TheirdaysidethermalradiationisaccessibletoSPITZER andhasevenbeendetectedfromtheground, revealingawealthofinformationabouttheiratmosphericthermalstructureandchemistry. I willpreviewthefirstpublicreleaseofprocessedlightcurvedatafromtheinitialyearoftheWASP project, whichwilltakeplacethisyear.

DesignchallengesintheconstructionofELTsColinCunningham (UK AstronomyTechnology

Centre)

TheEuropeanExtremelyLargeTelescopeisreachingcompletionofitsdesignphase. Likeanymajorproject, ithastobalancecost, riskandperformanceinordertobeaffordableonacompetitivetime-scaleandbeabletosatisfyambitioussciencegoals. I willdescribehowthisbalancehasbeenachievedwhilstmaintainingtheaspirationtobuildtheworld'slargestoptical/IRtelescopewithbuiltinadaptiveoptics. I willemphasizeUK rolesinaddressingtheconsiderablechallengesofdevelopingtheprimarymirrorconsistingof984segments, theadaptiveoptics

systems, andtheinstrumentsuite. Finally, I willshowsomeoftheexcitingprospectsforscientific,technologicalandindustrialbenefitstotheUK.

ProbingCosmologywiththeCMBRGeorgeEfstathiou (KavliInstituteforCosmology)

ThePlanckMissionwaslaunchedsuccessfullyinMaylastyear. I willgiveasummaryofthescientificaimsofthePlanckMissionandabriefoverviewofitscurrentstatus. I willalsoplacethePlanckmissionincontextwithgroundandsuborbitalCMB experimentsandotherprobesofearlyuniversecosmology.

TheEarlyStagesofStarFormationJenniferHatchell (UniversityofExeter)

Wheredostarsform? Howlongdoesittake?Whatcontrolstheirmasses? Thesequestionsandmorearebeingaddressedbymappingsurveysofmolecularcloudsatlongwavelengths(infraredandsubmillimetre), whichprovideacensusofdensecoresandthestarsformingwithinthem. Iwillshowhowtheadvancesintechnologywhichallowustomaplargeareasaremirroredinourincreasedunderstandingoftheearly, embeddedstagesofstarformation, andlooktowardsthefuturewithHerschelandSCUBA2.

TheHighEnergySunBobLin (Univ. ofCalifornia, Berkeley)

TheSunisthemostprolificandenergeticnaturalparticleacceleratorinthesolarsystem. Largesolarflaresarethemostpowerfulexplosionsinthesolarsystem, releasingupto ∼ 1032-33ergsin100-1000s, with &10-50%ofthisenergygoingtoacceleratingelectronsto ∼ 20 keV to ∼ 100sofMeV,andacomparableamounttoacceleratingionsto ∼ MeV to GeV energies. ImagingbytheRHESSI (RamatyHighResolutionSolarSpectroscopicImager)spacecraftofthehardX-ray(HXR)/γ−raycontinuumand γ−raylineemissionproducedbytheacceleratedelectronsandions,respectively, showthattheprocessofmagneticreconnectionunderliesboththeflareenergyreleaseandtheaccelerationofelectronsandions.InlargeSolarEnergeticParticles(SEP) events, ionsupto ∼ 100 GeV andelectronsupto ∼ 10sofMeV,wellintothegalacticcosmicrayenergyrange, aredetectedinsitunear1AU.Theseappeartobeacceleratedbycollisionlessshockwavesdrivenbyfast(&1000km/s)coronalmassejections(CMEs)withoforder ∼ 10 %ofthetotalCME energygoingintotheSEPs, thesameefficiencyasrequiredforsupernovashockstoaccelerategalacticcosmicrays. Themostcommon(&100s/monthnearsolarmaximum)solaraccelerationoccurshighinthecoronaandproducestheimpulsiveSEP eventsobservedintheinterplanetarymedium, thataredominatedby∼ 0.1 − 100 keV electronsandby ∼ 10 keV toMeV pernucleonionswithenormous(upto&10,000)enrichmentsintheisotope3Heandinultraheavyelements. Theaccelerationmechanismsare, atbest, poorlyunderstood;upcomingmissionsgoingclosetotheSun, suchasESA’sSolarOrbiter(∼ 0.28 AU) andNASA’sSolarProbePlus(∼ 9.5 solarradii), promisetoprovidekeyrelevantmeasurements.

TheESA CosmicVisionProgrammeMarkMcCaughrean (ESA)

I willpresentabriefoverviewoftheESA spacescienceandroboticexplorationprogramme,

42 Plenary

coveringmissionscurrentlyinoperation(includingHerschel, Planck, andRosetta)andthoseinpreparation(LISA Pathfinder, Gaia, JWST,BepiColombo, andtheExoMarsmissions). ThemajorityofmytalkwillconcentrateonthestatusandpromiseofthemissionscurrentlyunderstudyaspartoftheCosmicVisionprogramme, andtheroadmapfornewopportunitiesoverthecomingdecade.

PlasmaphenomenaonallcosmicscalesDonMelrose (UniversityofSydney)

I willgiveabriefhistoricalreviewofthedevelopmentofthefieldofplasmaastrophysics,emphasizingtheproblemsthatmotivatedthefield,andthenewplasma-physicsideasthatwereintroducedtoaddresstheseproblems. I willthendiscussthepresent-daystatusofthreegenericproblemsinplasmaastrophysics: 1. resonantscatteringandparticleacceleration; 2. coherentradioemissionmechanisms; and3. dissipationincollisionlessastrophysicalplasmas.

Proto-planetarydisksandplanetarymigrationRichardNelson (QueenMary, Universityof

London)

Thediscoveryofextrasolarplanetswithawiderangeoforbitalconfigurationssuggeststhatorbitalmigrationplaysafundamentalroleduringtheformationofplanetarysystems. DuringthetalkIwillreviewourcurrentunderstandingofplanetarymigration, anditsdependenceonthephysicalpropertiesofprotoplanetarydiscs, withtheroleofdiscthermodynamicsandturbulencebeinghighlighted. Modelsofplanetarysystemformationincludingmigrationwillbepresented.

GravitationalAstronomyBangaloreSathyaprakash (CardiffUniversity)

ThefirstdirectdetectionofgravitationalwavesareexpectedwithinthenextfivetosixyearswhenadvancedLIGO andVirgodetectorsbegintooperate. Thefirstdetection, whilealandmark, isonlythebeginningofwhatpromisestobeanewtoolforobservationalastronomy, cosmologyandfundamentalphysics. InmytalkI willdiscussthecurrentstatusofgravitational-waveobservationsandcapabilitiesoffuturedetectors. I willshowhowfutureobservationsmightimpactourunderstandingofastrophysicalphenomena(e.g.,neutronstars, blackholes, supernovae, GRGs),fundamentalphysics(e.g., matterunderextremeconditions, strong-fieldtestsofGR,darkenergy)andcosmology(e.g., cosmologicalparameters,blackholeseeds, stochasticbackgroundsfromtheearlyUniverse).

ExploringtheUniversewithGamma-RayburstsNialTanvir (UniversityofLeicester)

Thankstotheirextraordinaryluminosities, γ−rayburstscanbeseenatveryhighredshifts, andassuchprovidepowerfultoolsforexploringearlystructureformationandreionization.Spectroscopyoftheirafterglowsgivesredshifts,andpotentiallyalsoinformationaboutchemicalenrichmentoftheirhostsandthestateoftheintergalactic-mediumclosetotheburst.Identificationandcharacterisationoftheirfainthostsandneighbouringgalaxiesopensanewwindowongalaxyevolution. RecentlyGRB090423wasdetectedatredshiftz=8.2,highlightingthepromiseofGRBsforprobingtheveryhighredshiftuniverse. I willreviewthiswork

andotherrecentdevelopmentsinthefield,includingthestatusofhostgalaxysearches.

TheSWARM MissionKathyWhaler (UniversityofEdinburgh)

In1999, theInternationalUnionofGeodesyandGeophysicsadoptedaresolutiontoestablishanInternationalDecadeofGeopotentialFieldResearch, heraldingthestartofadecadeofcontinuousmonitoringofthemagneticfieldbynear-Earthorbitingsatellites, andimportantadvancesinspace-basedgravityfieldobservation.FormuchoftheInternationalDecade, multi-satellitevectormagneticobservationshavebeenavailable, leadingtomuchbettermodelsofthemainfieldanditsrateofchange, andimprovedunderstandingoftheinfluenceofmagnetosphericandionosphericfieldsonattemptstoisolatetheinternalfieldsignal. However, muchremainstobedone. Forinstance, evenduringtheparticularlyquietsolaractivityconditionsthathavecharacterisedmuchofthelastfewyears, andafterenormouseffortondataprocessingandselectionalgorithms, magnetosphericandionosphericfieldeffectsremainindatausedtoproduceinternalfieldmodels, sooursignalidentificationandseparationisfarfromperfect; 'comprehensivemodels'thatareintendedtoparameteriseandmodelknowninternalfieldsourcesandmagnetospheric/ionosphericcurrentsystemsarestillonlyappropriateformagneticallyquiettimes.However, thedemonstratedpowerfromhavingavailablesimultaneousmulti-satelliteinformationhasledtoESA approvalforasatelliteconstellationSWARM withintheEarthExplorerprogramme,scheduledforlaunchin2011. Inthistalk, I willdescribetheSWARM missiondevelopmentandanticipatedapplicationsofthedata, includinghowtheend-to-endsimulatorstudywasusedtoimprovetheconstellationdesignoverthatintheoriginalproposal, andthepotentialofSWARM forinvestigatingatmosphericprocessesrelatedtoclimateandweather, suchasspaceweatherandradiationhazards, aswellasthebetterdefinitionofthe'geological'magneticfieldsignalandnear-Earthexternalmagneticfields.

TheJamesWebbSpaceTelescopeGillianWright (UniversityofEdinburgh)

TheJamesWebbSpaceTelescope(JWST),thesuccessortoHubble, isalarge, 6.5mdiameter,infrared-optimizedspacetelescope, scheduledforlaunchin2014. ItwillhaveasuiteoffourinstrumentsdesignedtoenablewiderangingsciencefromthefirstluminousgalaxiesandgalaxyevolutiontotheformationofplanetsandtheevolutionofourownSolarSystem. InthistalkI describethesciencethemesthathavedriventheobservatorydesign, theenablingtechnologiesandtechnicalstatusofthemissionandtheinstrumentcapabilities, inparticularforthemid-infraredinstrumentMIRI.I willalsosummarisetheplansforoperations.

GalaxiesandStellarPopulationsRosieWyse (JohnsHopkinsUniversity)

I willdiscusshowstudyingresolvedstarsinthenearbyUniversecanbeusedtoinferconditionsathighredshift, tracehowgalaxiesevolveandconstrainthenatureofdarkmatter. Thisapproachiscomplementarytodirectstudyofsystemsathighredshift, butI willshowthatanalysisofindividualstarsallowsonetobreakdegeneracies,suchasbetweenstarformationrateandstellar

InitialMassFunction, thatcomplicatetheanalysisofunresolved, distantgalaxies.

P01ScaleSizeEvolutionofBrightestGalaxies

ClaireBurke (AstrophysicsResearchInstituteLJMU) with C. Collins, and J. Stott

Scalesizesofellipticalgalaxieshavebeenatopicofdiscussionrecentlyduetotheunexpectedresultthattheseobjectsevolvefromacompactstate.Wepresentourpreliminaryresultsofscalesizemeasurementsofbrightestclustergalaxies(BCGs)atz∼ 1, usingdeepimagingfromHST andSubaruMOIRCS of ∼ 10 BCGsinboththeopticalandnearinfra-red. WefindrobustBCG scalesizesof∼ 10kpc, andinferthatthisisevidenceformildsizeevolutionofthishomogeneouspopulationsincez∼ 1. Wediscussimplicationsofthisresult,inconcertwiththerecentresultofnomassevolutionofthesegalaxiesoverthesameperiod,forcosmologicalmodelsofthelatetimeevolutionofmassiveearlytypegalaxies.

Thecolours, AGN properties, environmentsandstarformationhistoriesofbulgedominatedpost-

mergersinthelocaluniverseAlfredoCarpineti (ImperialCollege)with

S. Kaviraj, and GalaxyZooteam

Galaxymergingisafundamentalaspectofthestandardhierarchicalgalaxyformationparadigm.InDargetal.(2010MNRAS.401.1043)wehavecreatedalarge, homogeneoussetofmergersthroughdirectvisualinspectionoftheentireSDSSusingtheGalaxyZooproject, apublicuserinterfaceontheworldwidewebforthemorphologicalclassificationofgalaxies. Atthetimeofwriting, over200,000volunteershavesubmittedover80millionclassificationsyieldingarobustcatalogueofaround3000mergerswhichhasbeenpresentedinDargetal. Weexploreasubsetofgalaxiesfromthiscataloguethatare'post-mergers', wheretheremnantappearstobeinthefinalstagesofrelaxation. Wefocusonpost-mergersthatshowevidenceforadominantbulge,makingthemplausibleprogenitorsofearly-typegalaxies. ForthissetofgalaxiesweexploretheirGALEX-SDSS UV/opticalcolours, AGN activity,localenvironmentsandstarformationhistories.64%ofourgalaxiesareeitherquiescentorshowLINER-likeemission, whiletherestareeitherstarforming(9%)orhaveSeyfertAGNs(25%). Wefindthattheplausiblemassratiosforthemergersthatcreatedthesesystemsarebetween1:1and1:10, withamedianvalueofaround1:3. Thespheroidalpostmergershavebluercoloursthanthegeneralellipticalgalaxypopulation, mostlikelyduetomerger-inducedstarformation.Comparisonwithstellarmodelssuggeststhatthestarformationactivityinmostofthesesystemspeakedlessthan1Gyrsago, suggestingthatsomeofstarformationrecentlydiscoveredinearly-typegalaxiesismerger-driven.

GalaxyClusteringUsingPhotometricRedshiftsLeonidasChristodoulou (UniversityofSussex)with

Jon Loveday, and GAMA Team

TheGAMA spectroscopicreleaseoffersauniqueopportunitytocalibratephotometricredshiftsfromSDSS downtor=19.4. TakingadvantageofthefactthatGAMA offersatrulyrepresentativesubsetofSDSS weconstructacatalogueof ∼ 5 million

Plenary–P01 43

objects, usinganartificialneuralnetwork(ANNz).Moreover, wecarryoutanextensiveerroranalysistocheckforpossiblebiasesinourredshiftsestimation. Wealsoshowindependentestimationsoftheunderlyingredshiftdistribution, usingaweightingmethod(Cunhaetal, 2009), whichrecoversmoreaccuratelytheredshiftdistribution.Thisallowsastorevealtheweaknessandthestrengthsofthetwomethods. Havingdonethat,wemeasurethetwopointangularcorrelationfunctioninluminositybinsandthenusingLimber'sapproximationwecalculatethespatialcorrelationfunction. Finallywecomparewiththeresultsintheliteraturefromspectroscopicsurveys.However, becauseoftheuseofphotometricredshiftsourworkextendstointrinsicallyfaintobjectswithmagnitudedowntoM=-14.

StudyinggalaxyevolutionwithFMOS (FibreMulti-ObjectSpectrograph)

EmmaCurtisLake (UniversityofOxford)withGavin Dalton, Thomas Mauch, Naruhisa Takato,

Naoyuki Tamura, Ian Smail, Philip Best,Jim Geach, David Sobral, and FMOS team

FMOS (FibreMulti-ObjectSpectrograph)isnowavailableontheSubaruTelescopeforobtainingnear-infraredspectraintheJ andH bands. With400targetfibres, withinawidefieldofview, thisinstrumentprovidesthemeanstoextendtheresultsfromlowredshiftspectroscopicsurveysusingthesamelinesasdetectedintheoptical. Inparticular, starformationcanbetracedbyH-αemissionbetween ∼ 0.5 < z < 1.7. I willgiveoverviewofFMOS andpresentinitialresults,includingspectroscopictargetingofHiZELS (High-Z EmissionLineSurvey)objects.

A newapproachtodisentanglingstarformationhistoriesfromsurveydata

IgnacioFerreras (UniversityCollegeLondon–MSSL)

Large, homogeneoussurveyssuchasSDSS orGAMA allowustoapplymultivariatetechniquesbasedatextractingdifferencesbetweenthestellarpopulationsofgalaxiesinamodel-independentway. InthistalkI willpresentrecentandongoingresearchfocusedonavolume-limitedsampleofearly-typegalaxiesfromSDSS.PrincipalComponentAnalysis(PCA) isusedtodefinetwoestimatorsofaverageageandrecentstarformationwhichisthenappliedtosubsamplesofclosepairsofearly-types(i.e. theprecursorsofdrymergers)ortosamplesclassifiedaccordingtothemassoftheparenthaloinordertoquantifytheeffectofenvironmentonthestarformationhistoryofgalaxies. Futuredirectionsforthepromisingfieldofmultivariateanalysisofphoto-spectroscopicdatawillbepresented.

A newsampleof"blazars"tostudytherelationshipbetweenradio-loudAGN andgalaxy

formationJenniferGupta (JodrellBankCentrefor

Astrophysics)with Ian Browne

Radio-loudactivegalacticnucleiarenowrecognisedtobevitalintheprocessofgalaxyformation, byprovidingfeedbackwhichregulatesthestar-formationprocess. Logicallyitfollowsthatinordertounderstandgalaxyformationandevolution, wemustunderstandAGN.However,thedetailsofhowAGN feedbackhappensisadifficultproblem; therearemanyunansweredquestions, suchaswhattriggerstheburstsofAGNactivity, howlongdotheburstsofactivitylastandhowdotheburstsevolve. Blazarsareasubsetof

radio-loudAGN whereoneoftheradiojetsisdirectedtowardstheobserveratasmallangletothelineofsight. Thereforeinblazarswegetthemostdirectviewoftherelativisticjetsthatmayultimatelyprovidethefeedback. Wehavedefinedanewsampleofnearbyblazar-likeobjects,attemptingtominimisetheselectioneffectsinordertounderstandthefundamentalandintrinsicpropertiesoftheseobjects. TheSurveyofExtragalacticNuclearSpectralEnergies(SENSE)samplecontains151compactradiocoreobjectswithin z < 0.2. HerewepresenttheSENSEsamplewithanemphasisonthewaysinwhichweareusingmultiwavelengthobservationsofthesampletoprobethephysicsofblazarsinthelow-redshiftUniverse.

GAMA photometryandtheCosmicSpectralEnergyDistribution

DavidHill (UniversityofStAndrews)withLee Kelvin, Simon Driver, Aaron Robotham, and

GAMA Team

Thecosmicspectralenergydistribution(CSED)describesthemeanradiationfieldwithinthesampledvolumeoftheUniverse. Itcangiveinsightintothestarformationhistory, andtheinitialmassfunction. Itsmeasurementrequiresaccuratephotometryfromanumberoffilters,whichhaspreviouslyledtodiscrepanciesbetweenopticalandNIR parameters. WeintroducetheGAMA photometricpipeline- amethodforgeneratingconsistentcoloursoverarangeofpassbands. WedescribethegenerationofGigapixelmosaicsandmatchedaperturecataloguesfromUKIDSS andSDSS data. Wequantifythesystematicoffsetsinbest-fittingluminosityfunctionparametersproducedbyusingdifferentaperturetypes, detectionthresholdsortotalmagnitudesystems. Finally, weintroduceaCSED,producedusingtheGAMA survey, andcompareittotheoreticalmodels.

Theradiospectralindexofsub-millimetregalaxies.

EdoIbar (UK AstronomyTechnologyCentre)withR.J. Ivison, P.N. Best, K. Coppin, A. Pope,

Ian Smail, and J.S. Dunlop

WehaveemployedtheGiantMetre-waveRadioTelescopeandtheVeryLargeArraytomaptheLockmanHole. At610and1400MHz, wereachnoiselevelsof15and6microJy/beam,respectively, withwell-matchedresolutions(∼ 5arcsec). Atthisdepth, weobtainedreliabledetectionsforabouthalfoftheknownsub-mmgalaxies(SMGs)inthefield(SCUBA,AzTEC andMAMBO).Forradio-identifiedSMGs, whicharetypicallyatz ∼ 2, wemeasureameanradiospectralindexof α(1400, 610) =-0.75±0.06(where Sν ∼ να)andstandarddeviationof0.29,betweenapproximaterest-framefrequenciesof1.8and4.2GHz. Theslopeoftheircontinuumemissionisindistinguishablefromthatoflocalstar-forminggalaxiesandsuggeststhatextendedopticallythinsynchrotronemissiondominatestheradiooutputofSMGs. CoolingeffectsbysynchrotronemissionandInverseComptonscatteringoffthecosmicmicrowavebackgrounddonotseemtoaffecttheirradiospectralenergydistributions. ForthoseSMGsjudgedbySpitzermid-infraredcoloursandspectroscopytohostobscuredactivegalacticnuclei(AGN),wefindacleardeviationfromtherestofthesample- theytypicallyhavesteeperradiospectralindices,α(1400, 610) . −1.0. Thesefindingssuggestthesemid-IR-/AGN-selectedSMGsmayhaveanintrinsicallydifferentinjectionmechanismfor

relativisticparticles, ortheymightresideindenserenvironments. Thisworkprovidesareliablespectraltemplatefortheestimationoffar-IR/radiophotometricredshifts, andwillenableaccuratestatisticalK-correctionsforthelargesamplesofSMGsexpectedwithSCUBA-2andHerschel.

Robustmethodstoprobesourceevolutioningalaxyredshiftsurveys

RussellJohnston (UniversityoftheWesternCape)

Oneofthemostfundamental, andstillrelevant,statisticalchallengesinmodernobservationalcosmologyisaccuratelydeterminingthegalaxyluminosityfunction. Determiningtheluminosityfunctionofgalaxiesremainsavitalandfundamentaltoolforassessingthestatisticalnatureofgalaxyformationandevolution. Pertinenttothisareaofstudyisaccuratelycharacterisingsourceevolutioningalaxyredshiftsurveys.

I willpresentarecentlydevelopedmethodthatrobustlyconstrainsluminosityevolutionarymodelsbyexploitingthepropertiesofthemagnitudecompletenesstestdevelopedbyRauzy(2001)andJohnston, Teodoro&Hendry(2007),combinedwithamaximumentropyapproach.Thisstatisticalapproachhasthepotentialadvantageovertraditionalapproachesbynotmakinganyassumptionoftheparametricformoftheunderlyingluminosityfunctionandisalsoindependentthespatialdistributionofgalaxies.

GAMA:SingleandMulti-ComponentGalaxyModelling

LeeKelvin (StAndrews)with Aaron Robotham,Simon Driver, Ewan Cameron, David Hill, and

GAMA Team

I presentresultsfromtheGAMA structuraldecompositionpipeline(GAMA-SIGMA;StructuralInvestigationofGalaxiesviaModelAnalysis)forallGAMA objectswithoptical-to-near-IR imagingfromtheSDSS &UKIDSS-LAS surveys. I showthatphotometricmodellingshorterthantheibandrestrictstherecoverabilityofgalacticproperties,anddiscusstheroleofdustinchangingourviewoftheUniverse. I alsodemonstratehowfullbulge-disk-bardecompositionisrequiredinordertogainfurtherinsightintotheformationandevolutionofgalaxies, anddiscussitsapplicationto ∼ 12,000nearbygalaxiesintheforthcominghigh-resolution/deepVST &VISTA imagingoftheGAMA fields.

TheALFALFA HI AbsorptionSurveyErinMacdonald (UniversityofGlasgow)with

Jeremy Darling, and ALFALFA Team

Wepresenttheresultsofawide-areapilotsurveytosearchforcoldNeutralHydrogen(HI) 21cmabsorptionutilizingtheAreciboLegacyFastAreciboL-BandFeedArray(ALFALFA) Survey. Thissurveyisthefirsttoconductawide-area(517.0deg2)''blind''searchforHI absorptioninthelocaluniverse. Thesurveyspans 10.9h < α < 14.95h

and +7.7◦ < δ < 6.3◦ centredontheVirgoCluster. ThefullALFALFA surveyisanHI emissionsurveythatcovers−650 ∼ km ∼ s−1 < cz < 17, 500 ∼ kms−1

(11% ofthisspanislosttoradiofrequencyinterferenceandGalacticHI emission)resultingina ∆z=0.054alongeachlineofsight. Whencompleted, theALFALFA surveywillspan7000deg2. OursurveyissensitivetoHI absorptionlinestowardsradiosourcesstrongerthan8.4mJy.Thisincludes8983sourcesforatotalsearchpathof ∆z = 485.1. Thereare243sourcestoward

44 P01

whichalldampedLy-α systems(N(HI) > 2 × 1020 cm−2)couldbedetected,and3282sourcestowardwhichN(HI) > 2 × 1021 cm−2 columnscouldbedetected. WedetectonepreviouslyknownHIabsorptionlineinUGC 6081, confirmingourmethodisfeasible, butmakenonewdetections.Usingthesedata, wecalculateanupperlimittotheHI columndensitydistributionfunctionanditsmoments. Thispilotsurveydemonstratesthevalueandfeasibilityoflarge-arearadioabsorptionlinesearchesthatarenotyetpossiblewithopticaltelescopesandprovidesabaselineforfutureHI 21cmabsorptionlinesurveysplannedfornewradiofacilities, suchasSKAMP,ASKAP,MEERKAT andtheATA.

ModellingtheUV/opticalFIR/submmemissionfromSpiralGalaxies

CristinaC.Popescu (JeremiahHorrocksInstitute,UCLan)with RichardJ. Tuffs

WepresentacomprehensivelibraryofspectralenergydistributionsofspiralgalaxiesintheMIR-submmrangecalculatedasafunctionofaminimalsetofphysicalparametersusinganupdatedandenhancedversionofthemodelofPopescuetal. (2000). Wedescribehowthissetofdust/PAH re-emissionSEDscanbeself-consistentlycombinedwiththeexistinglibraryofUV/opticaldustattenuationscalculatedusingthesamemodel(Tuffsetal. 2004)toinvertanobservedsetofbroad-bandphotometryofagalaxyspanningtheUV/optical- FIR/submmrangetoderivetheintrinsic(i.e. aswouldbeobservedintheabsenceofdust)UV/opticalemissionofthegalaxy. UsingrealandsimulateddataweillustratetheapplicationoftheSEDmodellingtechniquetothederivationofstarformationratesandstarformationhistoriesofopticallyselectedspiralgalaxiesinthelocalUniverseobservedbyGAMA andHerschel.Specifically, wequantifyhowtheamplitudeandwavelengthdependenceoftheUV/opticalattenuationisrelatedtotheamplitudeandcolouroftheFIR/submmcontinuumemissionmeasuredusingthePACS andSPIRE instruments, anddescribehowtoutilisemorphologicalinformationfromhigherresolutionopticalobservationsofGAMA galaxies(suchaslinearsizesofdisksandthebulge-diskdecompositions)intheinterpretationofthepanchromaticobservations.

RedandBlueSatelliteGalaxiesintheGalaxyandMassAssemblySurvey

MatthewPrescott (LJMU AstrophysicsResearchInstitute)with IvanK. Baldry, PhilA. James, and

GAMA Team

Theroleofblue-sequencesatellitegalaxiesinthefuellingofdiskgalaxies. A long-standingproblemfordiskgalaxiesistheoriginofthecontinuinggassupplyrequiredtoexplaintheirstarformationandchemicalabundanceproperties. Onepossiblesourceisfromgas-richsatellites, eitherthroughminormergers('cannibalism')orfromthegascomponentonlyofthedwarfbeingtransferredtothediskgalaxy, withthegasremovaloccurringeitherthroughtidesorthroughsupernova-drivenwinds. Aninitialsearchforgas-richcompanionsoffielddiskgalaxiesusingwide-fieldH αimagingshowsthatMagellanicCloud-likesatellitesaresurprisinglyrare. Thescarcityofgas-richcompanionscouldbeindicativeoftheefficiencywithwhichtheyhavebeengas-strippedandtransformedintored-sequence, passivedwarfs. InthistalkI willpresentthepreliminaryresultsofastudyonthered-to-blueratioofdwarfgalaxies

aroundisolatedfielddiskgalaxiesselectedfromtheGAMA survey, andthevariationinthisratioasafunctionofprojectedseparation.

AbundancegradientsinsimulatedgalaxydiscsAwatRahimi (UniversityCollegeLondon–MSSL)

with Daisuke Kawata, ChrisB. Brook,BradK. Gibson, and Carlos Allende-Prieto

TBC

GalaxyAndMassAssembly(GAMA):Thenextgenerationsurveyofsurveys.

AaronRobotham (StAndrews)with GAMA Team

TheGAMA surveyisthelatestgenerationphotometricandredshiftsurvey. ItwillcoverthefullSED ofgalaxies, fromtheFUV totheradio, andiscomplementedby130,000redshiftsobtainedfromtheAAT overa3yearperiod(finishingMay2010). GAMA willprobestructureoverthescalesof1kpcto1Mpc, helpingustounderstandgalaxyformation, theenergyoutputoftheUniverse, andtheroleofgroupsandclustersingalaxyevolution.

Modellingradiationfieldsingalaxiesusinganewradiationtransfercode

DmitrijSemionov (JeremiahHorrocksInstitute,UCLan)

Wedescribeanewraytracingradiationtransfer(RTR) codebeingdevelopedatUCLan, optimisedforcalculatingthedistributionofradiationfieldsindustygalaxies. PrimaryapplicationswillbetomodelimagesandintegratedSEDsindirectanddustre-radiatedlightofsyntheticgalaxiescalculatedselfconsistentlywithCDM cosmology.

NGC 2976&NGC 3351: 12CO(3-2)ObservationsanditsCorrelationwithPAH 8um

BoonKokTan (UniversityofOxford)withJamie Leech, Dimitra Rigopoulou, and NGLS

teammembers

Wepresent12CO(3 − 2) mapsofNGC 2976andNGC 3351obtainedusingtheJamesClerkMaxwellTelescope. BothgalaxiesarepartoftheNearbyGalaxyLegacySurvey(NGLS).Wecombinethesedatawiththe12CO(3 − 2) mapsfromNobeyamaRadioObservatoryandBerkeleyIllinoisMarylandAssociationinterferometertoderiveCO line-ratiomap. Thevalueof12CO(3 − 2) to12CO(1 − 0) lineratioweobtainedwaswithin0.2--0.6range. Usingthisratio, wederivedthetotalmoleculargasmassof3×107 solarmassforNGC 2976and7.55x108

solarmassforNGC 3351. Wepresentspectralmapsanddiscussthevelocityfieldandthevelocitydispersionofthetwogalaxies. WefindthatthesevelocitycomponentsareverysimilartothedatafromtheVLA surveyofHI emission.Using8umSpitzerdata, weinvestigatedthecorrelationofthe12CO(3 − 2) intensitywiththePAH 8micronsurfacebrightness. Westudytheradialdistributionofthesestarformationtracersinthetwogalaxiesandsuggestthatthecorrelationisgoodathighsurfacebrightnessregion. Weextendthisstudytoincludethetotalsurfacebrightnessofthe12CO(3 − 2) andthePAH 8 µmemissionof17galaxieswithintheNGLS samples. Wefindthatthecorrelationisverygoodatlargespatialscale, asbothphysicalparameterstraceactivestarformation.

P02Anultravioletstudyofthetheweakwind

probleminO starsMatthewAustin (UCL) with Raman Prinja

Learningthefinerdetailsaboutmass-lossfromstarsofearlyspectraltypeisimperative. Theimpactofthisenergeticphenomenonisgreat,acrossalargesliceofastrophysics. Recently,determiningtruemass-lossratesinO starshasbeenhamperedbydiscordantspectraldiagnostics.WedescribeanefforttocomputetherunofionfractionwitheffectivestellartemperatureforthewholeO starrange, forC,N,O,P,S andSi. WegivedetailsconcerningtheprojectundertakentofitC IV resonancelineprofilesinlateO dwarfsandhighlightthemagnitudeofthecurrentproblem.

ProbingSitesofMassiveStarFormation: TheMethanolMultiBeamSurvey

AdamAvison (JodrellBankCentreforAstrophysics)with Gary Fuller, James Caswell,

James Green, and MMB Collaboration

TheMethanolMultibeamsurveyisagalacticplanesurveyforClassII methanolmasersat6.7GHz. TheseuniquetracersofmassivestarformationhavebeenobservedusingapurposebuiltsevenbeamreceiverontheParkesradiotelescope, withhighresolutioncounterpartobservationstakenattheAustraliaTelescopeCompactArraytoachievehighaccuracypositions.

ThesouthernhemisphereobservationsisnowcompleteandthefirstcatalogueofMMB resultscoveringthegalacticcenterregion(345o-> 0o-> 6o)hasrecentlybeenreleased(Caswell2009).ThisalongwithacompletesurveyoftheLargeMagellanicCloud(Green2008)highlighttheinterestingresultsthesurveyisalreadyyielding.Workiscurrentlyongoingtocomparethelocationsofmassivestarformationsignpostedbythe6.7GHzmaserswithotherdataofthegalacticplanei.e. infraredsurveys(MIPS,GLIMPSE),excitedOH masersandsoontobetakenmolecularlineobservations. InthistalkI willaddressthelatestresultsoftheMMB surveyanditsfutureprospects.

SurveyoftypeIb/csupernovaprogenitorsinnearbystar-forminggalaxies.

JoanneBibby (UniversityofSheffield)withPaul Crowther

Pre-supernovabroad-bandimagingofgalaxieshasrevealedtheredsupergiant(RSG) progenitorofTypeII SNe. However, whilstWolf-Rayet(WR)starsarebelievedtobetheprogenitorofTypeIb/cSNeadirectobservationallinkisyettobeestablished. Bysurveying ∼ 10 nearbystar-formingspiralgalaxieswithVLT andGeminiweaimtoproduceacatalogueofWR starswhichcanbereferredtowhenaTypeIb/cSNeoccurs.

I summarizethenarrow-bandimagingtechniqueusedtoidentifyWR stars, alongwithMulti-ObjectSpectroscopyMOS) confirmation. I considerthelimitationsofground-basedimagingwithcomparisontoHST archivaldata. BydegradingthespatialresolutionofarepresentativesampleofLMC Wolf-Rayetstars, tothatofatypicalgalaxyinoursample, weaddressthequestionofcompleteness. WeaskwouldtheWR emissionstillbeobservedorwoulditbedilutedtothepointitwasnolongerdetectable?

P01–P02 45

Finally, I willdiscusscompletedsurveysinoursampleandhowtheyarebeingusedtoinvestigatewhetherthespatiallocationofdifferentWRsubtypescorrelateswiththelightdistributionofthehostgalaxy. Moreover, wecancomparethespatiallocationoftheWR starswithbothTypeIb/cSNeandGRBs.

A wide-field, high-resolutionviewofNGC2264JaneBuckle (UniversityofCambridge)with

J.S. Richer

Understandingthephysicsofwhereandhowstarsformisafundamentalastrophysicalquestion. Theprocessesassociatedwithstarformationareimportant: onlargescales, inthestructureandevolutionofgalaxies, tosmallscales, intheformationofplanets. Starformationoccursindensecoresinmolecularclouds, andmassivestarsforminclustersofmixedmassstars. Studiesofyoungclustersarethereforeessentialforunderstandingmassivestarformation.

NGC2264isanattractiveregiontostudy; at800pcitisoneofthenearestregionsofclusteredstarformation, andcontainstwoyoungprotoclusters.Oneoftheseisthoughttobeformingamassivestarof10-20solarmassesinthecentreofthecluster, fromthegravitationalmergerofintermediate-masscores.

Wepresentwide-field, highresolution2-D and3-D imagingofthisstarformingregioncovering1squaredegree, inUKIRT WFCAM H2narrow-band1-0S(1) lineemissionandJCMT HARP J=3-2CO emission. ThroughCO spectralimaging, wecanprovideacompletecensusofprotostellaroutflowactivityintheregion, investigatingthedynamicimpactoftheoutflowsonthenatalcloud. H2emissionhighlightstheyoungestflows,fromemissionarisingingasshockedbytheimpactofoutflows. Weusethisimagingdatatomeasuretheextentoftheveryyoungestflowsinthestarformingclusters.

Multiplegenerationsofmassivestarformationinclustercomplexes

SimonClark (OpenUniversity)with M. Messineo,H. Parsons, B. Davies, and M. Thompson

Theprocessesgoverningtheformationofmassivestarsarepoorlyunderstood, primarilyduetoobservationaldifficultiesresultingfromtheirrarityandhighextinction. Neverthelessitisthoughtthattheypredominantlyforminstaraggregates, whichinturnarefoundwithinlargerclustercomplexesassociatedwiththenatalGMC.Wepresenttheintialresultsofanextensivemultiwavelengthobservingcampaignaimedatconstrainingthestarformationhistoriesofsuchcomplexesandthepropertiesofthecoldprotostellarcoresandthe(proto-)stars/clustersfoundwithin, inordertoprovideconstraintsonthephysicsyeildingthem.

TheRMS Survey: NearInfra-RedSpectroscopyofMassiveYoungStellarObjectsInTheNorthern

HemisphereHeatherCooper (UniversityofLeeds)with RMS

Team

TheRMS surveyisthelargestcomprehensive,galaxy-widesurveyofmassiveyoungstellarobjects(MYSOs)todate. Colourcutsdefinedusing2MASS andMSX datawereusedtoselectmid-IR brightpointsourcesfromtheMSX satellitesurvey, producingaround2000candidateMYSOs.A seriesofmultiwavelengthfollow-upobservationshavebeendonetoclassifytheseobjectsandcharacterisetheMYSOsandH II regions. Asthe

finalstageofthisprocess, near-IR spectrahavebeenusedtodistinguishtheremainingH IIregions, oldstarsandothersourcesfromthegenuineMYSOs. Withthesenear-IR follow-upobservationscompleteinthenorthernhemisphere,andnearingcompletioninthesouthernhemisphere, thepreliminaryresultsandplansforexploitationofthenear-IR datawillbediscussed.

A MassiveStarisBorn: thecircumstellardisk,envelope, andbi-polaroutflowofW33A

BenDavies (RochesterInstituteofTechnology, NY)with S.L. Lumsden, M.G. Hoare, R.D. Oudmaijer,

and W.-J.de Wit

TheYoungStellarObject(YSO) W33A isoneofthebestknownexamplesofamassivestarstillintheprocessofforming. Wepresentnear-infraredhighspatialresolutionintegral-fieldspectroscopyofW33A,andfindevidencefor(a)arotationally-flattenedouterenvelopeataradiusofseveralthousandAU,(b)ahotcircumstellardiskataradiusof1-3AU,and(c)afastbi-polarionisedoutflowonsub-milliarcsecondscales, whichisalignedwiththeobject'slarger-scaleoutflow.Fromthekinematicsofthematerialintheinnernebula, wefindthatthecircumstellardiskorbitsacentralmassof > 10M⊙, whiletheouterenvelopeenclosesamassof ∼ 15M⊙. Theseresultsthereforeprovidestrongsupportingevidenceforthehypothesisthattheformationmechanismforhigh-massstarsisqualitativelysimilartothatoflow-massstars.

TheVLT-FLAMES TarantulaSurveyChristopherEvans (UK ATC)

30DoradusintheLargeMagellanicCloudisthelargestHII regionintheLocalGroup, providinganideallaboratoryforstudiesofstellarandclusterevolution. I willgiveanoverviewoftheVLT-FLAMES TarantulaSurvey, anESO LargeProgrammewhichhasobtainedmulti-epochopticalspectroscopyofover800OB-typestarsin30Dortoaddressfundamentalquestionsofmassivestarevolution, suchasmultiplicity, mass-loss, chemicalenrichmentviarotation, andclusterdynamics.

TypeIbcsupernovaeindisturbedgalaxies:evidenceforatop-heavyIMF

StaceyHabergham (AstrophysicsResearchInstitute)with J.P. Anderson, and P.A. James

Wecomparetheradiallocationsof169core-collapsesupernovaetotheR-bandandH αlightdistributionsoftheirhostgalaxies. Whenthegalaxiesaresplitinto'disturbed'and'undisturbed'categories, astrikingdifferenceemerges. Thedisturbedgalaxieshaveacentralexcessofcore-collapsesupernovae, andthisexcessisalmostcompletelydominatedbysupernovaeoftypesIb,IcandIb/c, whereastypeII supernovaedominateinallotherenvironments. Thedifferencecannoteasilybeexplainedbymetallicityorextinctioneffects, andthusweproposethatthisisdirectevidenceforastellarinitialmassfunctionthatisstronglyweightedtowardshighmassstars,specificallyinthecentralregionsofdisturbedgalaxies.

High-MassX-rayBinariesintheNIR:Orbitalsolutionsoftwohighlyobscuredsystems.

AndrewMason (OpenUniversity)withA.J. Norton, J.S. Clark, I. Negueruela, and P. Roche

I presentNIR spectroscopyobtainedusingtheVLTandISAAC oftwoeclipsingX-raypulsars, OAO

1657-415andEXO 1722-363. Bothofthehigh-massdonorstarsinthesesystemshaveonlyrecentlybeendiscovered, duetotheirhighlevelsofextinction. I willinitiallydiscussourworkinspectrallyclassifyingthetwodonorstars. ThedonorintheEXO 1722systemwasfoundtobeatypicalofthisclassofHMXB.ThedonorwithinOAO 1657wasfoundtobeamoreevolvedOfpe/WN9star. TheseresultsthrowlightontheunusualpositionofOAO 1657-415intheCorbetdiagram. Wehaveconstructedradialvelocitycurvesforbothofthesesystems, andI willpresentorbitalsolutionsandthefirstNS massdeterminationsmadeutilisingNIR spectroscopyforeachsystem.

TheevolutionofthepeculiarvariableV838Monocerotis2002-2009

MarkRushton (JeremiahHorrocksInstitute,UCLan)with M.T. Rushton, T.R. Geballe, A. Evans,

and S.P.S. Eyres

ThepeculiarvariableV838Monocerotiswasdiscoveredineruptionin2002andtransformedfromaK-typestarintothecoolestknownsupergiant. Sincethen, itsnear-infraredspectrumhasbeendominatedbystrongmolecularbands,andisreminiscentofthatofanL-typebrowndwarf. However, V838Moncontinuestoevolverapidly. Wepresentnear-infraredspectroscopyoftheobjectobtainedonmultipleoccasionsbetween2002and2009, showingthechangesthathaveoccuredinthatperiod. ThecauseoftheoutburstofV838Monisuncertain, butthediscoveriesofaB-typecompanionandanearbyclusterofstarsshowstheobjectistooyoungforanova, oraverylatethermalpulse. Theleadingexplanationisastellarmerger.

P03DoBBF eventscontributetoinnermagnetospheredipolarisation? A threeyearstatisticalstudyusingconcurrentClusterandDoubleStarobservationRogerDuthie (UniversityCollegeLondon–MSSL)with Andrew Fazakerley, Iannis Dandouras, and

Elizabeth Lucek

TheobserveddynamicalphenomenonofflowinEarth’smagnetotailwhichisintermittent, high-speed&non-fieldalignedistermed“burstybulkflow”(BBF).Dipolarisationofthemagneticfieldwithinthenight-sidemagnetosphereofEarthmaybecausallylinkedtoBBFs. BothphenomenaareattributedtotheEarth'ssubstormcycle.Competingmodelsattemptingtoexplainsubstormprocesses, andthecausallinkbetweenBBF anddipolarisation, havestilltobeconclusivelyverifiedorfalsified. Thesearechieflythecurrentdisruption(Lui1991)&near-Earthneutralline(Bakeretal1996)models. A statisticalstudyhaspreviouslybeenperformed(Takadaetal2006)throughconcurrentobservationsbyCluster4(“Tango”)&DoubleStarTanCe1, makinguseofmagnetotaildatafromoneyear. ItwasfoundfromthisthatathirdoftheBBF eventsdetectedbyCl4hadwiththemanassociateddetectionofadipolarisationeventbyTC1. Thestatisticalresultssuggestedthatthespacecraftseparationwasgenerallyshorter, andthemagneticfieldatTC1typicallyhadasmallerpolarcomponent, whenassociationbetweendetectionswasfound.Additionally, near-geosynchronousregion(R ∼ 6.6RE )dipolarisationstendednottohaveanassociationwithBBF eventdetections. The

46 P02–P03

presentstudyextendsthetimeintervaltothreeyears. ThefindingsfromtheobservationofBBF &fielddipolarisationscantherebybefortifiedandimproved. Issuesraisedbythepreviousstudycanbealsobemorefullyaddressed.

Lui(1991)A synthesisofmagnetospherissubstormmodels, J.Geophys. Res., 96, 11,389-11,401Bakeretal(1996)Neutrallinemodelofsubstorms;Pastresultsandpresentview, J.Geophys. Res.,101, 4967-4989Takadaetal(2006)DoBBFscontributetoinnermagnetospheredipolarizations:ConcurrentClusterandDoubleStareobservations,Geophys. Res. Lett., 33, L21109

AveragepropertiesofthemagneticreconnectioniondiffusionregionintheEarth’smagnetotail:

2001–2005Clusterobservationsandcomparisonwithsimulations

JonathanEastwood (ImperialCollegeLondon)with T.D. Phan, M Oieroset, and M.A. Shay

CollisionlessmagneticreconnectionplaysakeyroleinthedynamicsoftheEarth’smagnetosphere.Ofparticularimportanceisthediffusionregion,sincethisiswherethemagneticfieldultimatelyreconnects. Althoughconsiderableprogresshasbeenmadeinrecentyears, manyquestionsremain, inpartbecauseitisdifficulttomakein-situobservationsofthisregion, andsorelativelyfewindividualeventshavebeenreportedintheliterature.

Toaddressthisproblem, theClustermagnetotaildatasetfrom2001- 2005(constituting175magnetotailpasses)hasbeencomprehensivelysurveyedforencounterswithreconnectionsitesintheplasmasheetbysearchingforcorrelatedreversalsinthenormalmagneticfieldandtailward/earthwardplasmaflow. Thissurveyresultedin33events. Oftheseevents, 23(70%)wereinqualitativeagreementwiththeexpectedpatternofHallfields, indicatingadiffusionregionencounter. Withinthesetofdiffusionregionencounterscorrespondingtoanti-parallelreconnection, theabsolutesizeofboththeHallelectricandmagneticfieldwerebothfoundtovaryfromeventtoevent. However, withappropriatenormalizationtotheobservedboundaryconditions, consistentmagnitudesofboththeaveragepeakHallmagneticandtheaveragepeakHallelectricfieldarefound. Tobetterunderstandthisexperimentaldata, largeparticle-in-cellsimulationswereperformed,normalizedinthesamewayasthedata. Acomparisonoftheobserveddataandthepredictionsofsimulationswillbeshown.

TheseresultshelptoestablishtheoccurrencerateofdiffusionregionsrelativetomacroscopicsignaturesandtheaveragepropertiesofthediffusionregionintheEarth'smagnetotail. Wealsodiscussthemostusefulsignaturesforestablishingexperimentallythein-situmeasurementofdiffusionregions.

10YearsofCluster: HighlightsofMulti-pointMeasurementsinSpacePlasmas

C.PhilippeEscoubet (ESA/ESTEC) withM.G.G.T. Taylor, A. Masson, H. Laakso, and

M. Goldstein

Afteralmost10yearsofoperations, theClustermissionisfulfillingwithgreatsuccessitsscientificobjectives. ThemaingoaloftheClustermission,madeoffouridenticalspacecraft, istostudyinthreedimensionsthesmallandmedium-scaleplasmastructuresinthekeyplasmaregionsoftheEarth’senvironment: solarwindandbowshock,

magnetopause, polarcusps, magnetotail, andauroralzone.

Duringthecourseofthemission, therelativedistancebetweenthefourspacecrafthasbeenvariedfrom100to10,000kmtostudythescientificregionsofinterestatdifferentscales.Sincesummer2005, newmulti-scaleconstellationshavebeenimplemented, wherethreespacecraft(C1, C2, C3)areseparatedby10000km, withthefourthone(C4)atavariabledistancefrom40to10000kmfromC3.

Wewillhighlightsomeofthemainresultsfromthelast10years: evolutionofblackauroras, firstdirectmeasurementsofelectriccurrents,observationofthelargestreconnectioneventof2.5millionkminlength, observationsofgiganticsurfacewaves, firstevidenceofreconnectioninturbulentplasmaandusageofinterferometrytolocaliseelectromagneticemissions. ThepresentationwillalsocoverClusterdataaccessibility, throughtheClusterScienceDataSystem(CSDS) andtheClusterActiveArchive(CAA) whichwasimplementedtoprovideapermanentarchiveofhighresolutionClusterdatafromallinstruments.

Multi-spacecraftobservationsofauroralelectronaccelerationbyCluster

ColinForsyth (UniversityCollegeLondon–MSSL)with A.N. Fazakerley, A.P. Walsh, K. Garza,

C.J. Owen, I. Dandouras, K-H. Fornacon, andE. Lucek

DuringrecentyearstheorbitoftheClusterspacecrafthasevolvedsuchthatthespacecraftpassthroughtheauroralaccelerationregionclosetoperigeeduringthedaysideseason. Thispresentstheopportunitytomakemulti-spacecraftmeasurementsofthisregionforthefirsttime.

WepresentacasestudyofanupwardauroralcurrentregionobservedbyClusterinDecember2009. Duringthisevent, Cluster1andCluster3wereapproximatelylocatedonthesamemagneticfield-linebutseparatedby1000km. Weshowthattheelectronpopulationwasacceleratedalongthefield-linebetweenCluster1and3. Magneticfieldobservationsconfirmthepresenceofanupwardcurrentsystem. Basedontheseobservationsweestimatethesizeofthelengthoftheaccelerationregion.

ExtendingClusterJSOC scienceoperationsoverthepasttenyears

MikeHapgood (STFC RutherfordAppletonLaboratory)with M.G. Hutchinson,

M.A. Hapgood, T.G. Dimbylow, P.A. Chaizy, andA. McDermott

JSOC hassuccessfullyco-ordinatedthescienceoperationsofESA'scornerstoneClustermissionfortenyears. Theoriginalmissiondurationwastwoyearsandextendingthescienceoperationsbeyondthisperiodhasbeenatechnicalandmanagementchallenge, especiallyasthespacecraftandinstrumentsage, andstaffleaveandarereplaced. Furthermore, thesciencegoalsofClusterhaveevolvedinresponsetoscientificadvancesandtonewscientificopportunities(providedbyorbitalevolutionandbycollaborationwithnewexperimentsinspaceandontheground). Meetingthesechallengeshasbroughtconsiderableimprovementsandpositiveinsightsinco-ordinatingscienceoperations,includingthestructuredspreadingofexpertisewithintheteamtominimiseriskandincreaseflexibilityaswellasbuilding-inincreased

automationandimprovedsafetycheckingviarule-basedplanningtechniques. Importantly, expertisehasbeengainedinthetheoreticalandpracticaldevelopmentanduseofgenericplanningconceptsandsystemsaimingatimprovingthescientificreturnandthecostefficiencyofspacesciencemissions, includingmulti-pointmissions.

UsingCluster’sobservationsofthesolarwindtoinvestigatecollisionlessplasmaturbulence--

currentresultsandoutlookforthefutureKhuromKiyani (UniversityofWarwick)with

A. Turner, S.C. Chapman, B. Hnat,Yu. V. Khotyainstev, and F. Sahraoui

In-situobservationsofmagneticfluctuationsinthesolarwindshowan‘inertialrange’ofMHDturbulence, andathigherfrequencies, across-overtoscaleswherekineticeffectsbecomeimportant.Thiscrossoverisseeninthepowerspectraldensity(PSD) asasecondbroad-bandpowerlawregionextendingfromthetypicalionLarmorscaleofthesystemtoelectrongyroscales. Theoreticalstudiesofplasmaturbulencepredictthenatureofthescalinginthisregioncentredaroundpredictionsofthespectralslopeandassociatedscalingexponents.

Wepresentresultsfromhigh-frequencymagneticfielddatafromClusterinintervalswherethespacecraftwereinquasi-stationaryambientsolarwindandtheinstrumentswereoperatinginburstmode. Themagneticfielddataarefromthefluxgateandsearch-coilmagnetometersfromtheClusterFGM experiment(∼ 67Hz), andtheSTAFFexperiment(∼ 450 Hz). Thesedatasetsprovideobservationsofthissecondscalingrangeovertwodecadesinfrequency. Thishighcadenceallowsaprecisedeterminationofthestatisticsatthesesmallscales.

WeperformarobustmultiscalestatisticalanalysisfocusingonthePSD,PDFsoffieldfluctuations,higher-orderstatisticstoquantifythescalingoffluctuations; aswellasdescribingthedegreeofanisotropyinthefluctuationsparallelandperpendiculartotheaveragelocalmagneticfield.

Thestudyofsolarwindturbulencepresentssomechallengestosomerecentandfuturemissions.CurrentlyClusterstillpossessessomeofthebestaccessibleobservationsofkineticscaleelectromagneticwaveforms–evenafter10years.Toanswertheopenquestionofhowcollisionlessturbulenceisdissipatedintoheatingthesolarwind, weneedtopushfurtherthetelemetryandsensitivityofmeasurementsfromfuturemissions.WeconcludebydiscussingthesourcesoferrorfrominstrumentnoiseandouroutlookonhowClustercaninformfuturemissions.

Here, thereandeverywhere: gettingafeelforboundarylayerevolutionusingmultipoint

measurementsMattTaylor (EuropeanSpaceAgency)with I.J. Rae,

C. Watt, K. Nykyri, B. Lavraud, A.N. Fazakerley,M.W. Dunlop, A. Borg, H. Laakso, C.P. Escoubet,A. Masson, M.N. Nishino, M. Lester, S.E. Milan,J.A. Davies, L. Kistler, C. Mouikis, M. Volwerk,

A. Grocott, C. Forsyth, A.P. Walsh, A. Lui, C. Shen,Z. Pu, and J. Shi

Onthe11thJuly2006, duringaperiodofnorthwardIMF,theGeotail, DoubleStar1andClusterspacecraftallcrossedthemagnetopauseregionwithin2hours(UT) ofoneanotherwhileseparatedbymanyhoursinlocaltime. Duringthistimelarge-scaleoscillationswereobservedinbothgroundbasedandspacecraftdata. Weutilize

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thesenumerousmeasurementstoexaminetheextentandevolutionoffluctuationsinandaroundthemagnetopauseboundarylayer. ThisworkisbeingcarriedoutaspartofanInternationalSpaceScienceInstitute(ISSI) workinggroupon‘ComparativeCluster- DoubleStarmeasurementsoftheMagnetotail’.

TheMagnetotailPlasmaSheetRevisited: ClusterPEACE Statistics

AndrewWalsh (UniversityCollegeLondon–MSSL) with A.N. Fazakerley, C. Forsyth, and

C.J. Owen

WiththeClusterActiveArchivenowcontainingalargevarietyofhigh-quality, validateddataproducts, thereisanopportunitytocarryoutlarge, multi-instrumentstatisticalstudiesusingClustermeasurements. Wepresentfirstresultsfromonesuchstudy: asurveyofelectronpitchangledistributionsmeasuredbyClusterPEACEduringthe2002tailseason(July- October). Intotal ∼ 850,000distributionshavebeenexaminedintermsofmagneticfieldstrength, auroralindicesandotherparameters. Wefindthatthemagnetotailplasmasheetisonlyroutinelyisotropicwhen|B| < 3nT,i.e. closetotheneutralsheet. Outsidethisregionalow-energyfield-alignedpopulation, presumablythatidentifiedbyAsnesetal. (2008), waspresentatalllevelsof|B|.Significantelectronfluxeswerefoundtoextendtohigher|B|athigherAL/AE andexhibitedenergy-dispersedbehaviouratthehigh|B|edge. TheslopeofthisdispersionalsochangedwithAL/AE.

P04X-rayBrightPointTopologyStudywithHinode

andSTEREOCarolineAlexander (JeremiahHorrocksInstitute,

UCLan)with R.W. Walsh, M. Marsh,R.C. Maclean, and G. DelZanna

Wepresentacasestudyofamediumsized(∼ 15")X-raybrightpointobservedwithHinodeandSTEREO.Wehavestudiedtheevolutionandtopologythroughoutitslifetimeandpresentresultsonphysicalcharacteristicsaswellasstructure.Thetopologyhasbeenstudiedusingavarietyofmethods. PotentialfieldextrapolationshavebeencarriedoutandcomparedwithX-rayimagesfromXRT.Edge-detectionimageprocessinghasthenbeenusedonXRT imagestoseeifthisclarifiesanyloopstructurepresent. STEREO datahasalsobeenusedtoexplorethe3D topologyandinvestigatewhatline-of-sighteffectshaveonpreviousresults.

PlasmaMotionsandMagneticReconnectionHeatinginthe2007, May19Flare

LenCulhane (UniversityCollegeLondon–MSSL)with H. Hara, T. Watanabe, L.K. Harra, and

P. Young

WereportobservationstakenwiththeHinodeEISspectrometerofaloop-tophotsource, anearbyfastjetandaninflowtothehotsourceregionduringtheimpulsivephaseofalongdurationGOES ClassB9.5flareon2007, May19. TheeventwasalsoobservedwiththeHinodeSolarOpticalandX-rayTelescopes(SOT,XRT),RHESSIandTRACE.Intheimpulsivephase, EIS wasscanningaregionaboveFeXVII (192Å) andCaXVIII (255Å) emittingloopsatT ∼ 5 MK withasmallcusp-shapedapex. Theregionabovetheloopshas12MK hotplasmacomponentsthat

wereobservedinFeXXIII (263Å) andFeXXIV(192Å,255Å) emissionandintheRHESSI 4–6keV band. Atthepeakoftheimpulsivephase, thishotthermalsourceshowedexcesslinebroadingindicatingnon-thermalvelocitiesof ∼ 100 km/sandaweakredshiftof ∼ 30 km/s. A blue-shiftedjetwithaDopplervelocityof200km/sisalsoobserved. ThereisalsoacoronalstructureseeninFeXII 195Å emissionwithmaterialflowingintothehotsourceregionat ∼ 20 km/s. Twonon-thermalhardX-raysourcesareseenwithRHESSIinthe15–40keV band. Oneincludesbothoftheflaringloopfootpointswhiletheotherisfoundabovethelooptop. Alloftheseobservationsareconsistentwiththelocationofamgnetticreconnectionsitenearthehotsourceregionandthecusp.

Hinode/EIS observationsofactiveregionloopsGiulioDelZanna (UniversityofCambridge)

NewmeasurementsofelectrontemperaturesanddensitiesinactiveregionloopsobtainedwiththeHinode/EIS spectrometerarepresented. Theyareobtaineddirectlyfromlineratiosandnewatomicdata. ThesemeasurementsarecomplementarytothosepreviouslyobtainedonDopplermotions,and, oncerefined, willallowdetailedcomparisonswithresultsfromtime-dependentmodelling. Newobservationalandtheoreticalchallengesarebrieflydiscussed.

ObservationsofflareribbondensitiesusingHinode/EIS

DavidGraham (GlasgowUniversity)withLyndsay Fletcher

WepresentnewhighcadencemeasurementsofplasmadensityandbulkflowvelocitiesinasolarflareusingobservationsfromHinode/EIS andTRACE.Wehavefoundapparentdensityenhancementsinchromosphericflareribbonsandfootpoints, derivedusinglineratiosinFeXII,FeXIII andFeXIV.Bycombiningthesewithco-spatialvelocitymeasurements, weseesignsofcompressionandexpansionoftransitionregionandchromosphericplasma, inresponsetotheflareenergyrelease. Amongtheseobservationsaredensityenhancementslastingwellintothedecayphaseoftheflare, andsignsofasymmetricalblueandredshiftsacrossfootpoints. Wefindthatthehighcadenceandwidewavelengthrangeofthisdataisparticularlysuitedtoflarestudies, andrecommendthemforfutureobservingcampaignsinthenewsolarcycle.

WhatcanHinodeobservationstellusabouteruptionsfromsigmoidalactiveregions?

LucieGreen (UniversityCollegeLondon–MSSL)

SoftX-rayimagesoftheSunhaveshownthatsomeactiveregionscontainloops, orcollectionsofloops, whichappearforwardorreverse"S"inshape. Thesestructuresareknownassigmoidsandareofinterestbecausesigmoidalactiveregionshaveahighprobabilityofproducinganeruption. Recentobservationalandtheoreticalworkhassupportedtheinterpretationofthemagneticstructureofsomesigmoidsasbeingthatofafluxropelyingverylowinthesolaratmosphere, havingabaldpatchseparatrixsurfacetopology. Thisworkindicatesthatthefluxropeispresentinthesolaratmospherebeforetheonsetoftheeruption. Themainquestiontobeaddressednowishowthesigmoidalactiveregionswhichproduceaneruptionevolvetowardaninstabilityorlossofequilibrium.

WeuseHinodeobservationstoinvestigateeruptivesigmoidalactiveregions. Wediscusstheimportanceoftheevolutionofthephotosphericmagneticfield, theroleofreconnectionandpresentresultsfromEIS whichgiveaninsightintohowthesigmoidandoverlyingarcadefieldevolvetowardtheonsetofaneruption.

RegularizedinversiontechniquesforrecoveringDEMsfromHinode/XRT data

IainHannah (UniversityofGlasgow)withL. Braidwood, and E.P. Kontar

HinodeXRT providesunprecedentedspatialresolutionknowledgeoftheplasmatemperaturedistributionresultingfromheatinginthesolaratmosphere. However, theinferenceoftheDifferentialEmissionMeasureDEM(T) fromXRTrawdataisanill-posedinverseproblem. Here, wedevelopandapplyanenhancedmodel-independentregularizationalgorithmusedinRHESSI X-raysoftwareforthisprocessmakinguseofgeneralconstraintsontheformoftheDifferentialEmissionMeasures. Thealgorithmnaturallyprovidessignaldependentresolutionofthemethodthusgivingaclearcriteriatodeterminewhethertheplasmaisconsistentwithanisothermalmodel. Itcanalsobeeasilyadaptedtoworkwithothersolarmulti-filterdatasuchasSDO/AIA

WeshowbysimulationsthatthistechniqueyieldsDEM(T) withconsiderablymoreinformationandhigherqualitythanpreviousalgorithmsandapplythemethodtoXRT multi-filterobservationsofactiveregions.

Whatcantheorydoforyou?AlanHood (UniversityofStAndrews)

Analyticalapproximationsandnumericalsimulationsarefrequentlyusedtomodelvarioussolaratmosphericphenomena. Theseresearchtopicsareoftendrivenbythelatestobservations.A briefdescriptionofsomeoftheUK'srecentadvancesintheorywillbepresented, indicatingwherethedirectionthetopicsarelikelytotakeinthefuture. Theaimofthistalkistostimulateadiscussionofwhatobservationsareneededtodeveloptheoreticalmodelsfurther.

Coronalsignaturesofasunspotlight-bridgeSarahMatthews (UniversityCollegeLondon–

MSSL) with Deborah Baker, andSantiagoVargas Dominguez

Sunspotlight-bridgesarebrightlanesofmaterialthatdividetheumbra. Theirappearancesignifiesthereestablishmentofthegranulationwithinthespot, andoftenindicatesthebeginningoffragmentationofthespotitself. Theincreasedbrightnessofthelight-bridgerelativetothesurroundingumbraisaclearindicationthattheplasmatemperatureinthisregionishigher. Ithasalsobeennotedthatlight-bridgesoftenshowenhancedchromosphericactivity, withHα surgesandchomosphericjetsreportedinanumberofcases(e.g. Bhartietal. 2007, Shimizuetal.2009). Berger&Berdyugina(2003)alsofoundaconstantbrightnessenhancementabovealight-bridgeinobservationsinthe1600 ApassbandoftheTransitionRegionandCoronalExplorer(TRACE),whileKatsukawa(2007)foundthatlight-bridgeformationwasspatiallyandtemporallycoincidentwiththeheatingof ∼ 1 MK loopsasobservedbyTRACE.Light-bridgesthusseemtohavearoleinreleasingmagneticenergystoredinthespotaswellasinitsdecay. Inthisworkwe

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useobservationsfromHinodeandSTEREO toinvestigatetheextenttowhichthepresenceofasunspotlight-bridgeaffectstheoverlyingtransitionregionandcorona. Inparticularwecommentonchangesinthecoronalvelocityfieldinconnectionwithactivityintheunderlyingphotosphereandcorona.

Relationshipbetweenmagneticfieldandcoronaloutflowsinactiveregions

RobertO'Neil (UniversityCollegeLondon–MSSL)with LouiseK. Harra, and DavidR. Williams

OutflowsfromtheedgesofactiveregionshavebeenobservedwithHinodeEIS.Itisexpectedthattheseoutflowsareoneofthesourcesoftheslowsolarwind. Thephysicalmechanismproducingtheoutflowsisasyetunclearwithvarioussuggestionsbeingputforward(e.g. compression(Murrayetal.), magneticreconnection(Harraetal.), quasi-separatrixlayers(Bakeretal.). Inordertoprogresstheunderstandingofoutflowsfurther,astatisticalstudyhasbeencarriedouttodeterminetherelationshipbetweenmagneticfieldandtheoutflowspeeds. Thisencompasseshowtheflowsevolvewithtime. Wewillpresentpreliminaryresultsanddiscusstheimplicationoftheserelatedtoslowsolarwindformation.

Activeregionmoss: basicphysicalplasmaparametersandtheirtimevariability

DurgeshTripathi (UniversityofCambridge)withHelen Mason, GiulioDel Zanna, and Peter Young

Wepresentastudyofthephysicalplasmaparameterssuchaselectrontemperature, electrondensity, columndepthandfillingfactorsinthemossregionsandtheirvariabilityoverashort(anhour)andalongperiod(5consecutivedays)oftime. Primarily, wehaveanalyzedthespectroscopicobservationsrecordedbytheExtreme-ultravioletImagingSpectrometer(EIS)aboardHinode. InadditionwehaveusedsupplementaryobservationstakenfromTRACEandtheX-RayTelescope(XRT).WefindthatthemossemissionisstrongestintheFexiiandFexiiilines. BasedonanalysesusinglineratiosandemissionmeasurewefoundthatthemossregionhasacharacteristictemperatureoflogT =6.2.TheelectrondensitiesmeasuredatdifferentlocationsinthemossregionsusingFexiiratiosareabout1-3×1010 cm(-3)andabout2-4×109

cm(-3)usingFexiiiandFexiv. Theelectrondensitysubstantiallyincreases(byafactorofabout3-4orevenmoreinsomecases)whenabackgroundsubtractionwasperformed. Thedensityandtemperatureshowverysmallvariationovertime. BycombiningtheobservationsrecordedbyTRACE,EIS andXRT,wefindthatthemossregionscorrespondtothefoot-pointsofbothhotandwarmloops.

ConvectiveplasmaaroundsolarporesSantiagoVargasDominguez (UniversityCollege

London–MSSL)

Magneticstructuresarecommonlyobservedinthesolarphotosphereatmanydifferentspatialscales,beingsunspotsandporesthemostconspicuousones. Theformation, morphologyandevolutionofmagneticfeaturesareintenselylinkedtosolaractivityfromthephotospheretothecorona.Convectiveplasmaandembeddedmagneticfielddeterminethedevelopmentofdifferentstructuresbutthereisnotclearconsensusfromamodelexplainingthetransitionfromporesintosunspots.Plasmaflowsinsolaractiveregionscangiveusaclueontheongoingprocessesandinteractions

leadingtotheformationofthesemagneticstructures, i.e. theformationofpenumbraearoundanumbralcore. Inthepresentworkwefollowtheevolutionofsolarporesfromhigh-resolutiontimeseriesofimagesbycomputinghorizontalpropermotions. Weaimatdeterminewhetherornotwefindevidencesofthepresenceofstronglargeoutflowsaroundpores, asinthecaseofsunspots,andhowtheplasmaflowsareaffectedintimebytheevolutionofthepores.

P05FRODOSpec: RoboticSpectroscopyusingthe

LiverpoolTelescopeRobertBarnsley (LJMU) with I.A. Steele

FRODOSpec(Fibre-fedROboticDual-beamOpticalSpectrograph)isanewbench-mounted,integralfieldunitspectrographcurrentlyavailabletousersofthe2mroboticLiverpoolTelescopeonLaPalma. I presentdetailsofthespectrographandalsotheautomatedpipelinereductionprocesswhichdistributestheresultingdatatotheend-userinanarrayofdifferentformatsincludingaonedimensionalarc-fittedspectrum. Weanticipatethattheautonomousnatureofthetelescopecombinedwiththeautomatedreductionprocedurewillbringnewdevelopmentsintheareasofrapidresponseastronomy, suchasGRBs,wherequickidentificationisessentialtoobtaininggoodqualityfollowupdata.

A studyoftheSuperWASP detectormapsJoaoBento (UniversityofWarwick)with

Peter Wheatley

TransitingplanetsurveyshavebecomeincreasinglypopularsincethefirstdiscoveryofaplanetarytransitaroundHD209458usingasmallandinexpensivewidefieldtelescope. Motivatedbythisresult, TheSuperWASP projectwasfounded, consistingof2robotictelescopesaimedatsurveyingthenightskyinsearchofplanetarytransits. Aswithmostgroundbasedsurveys,systematicnoiseisalimitingfactorinprecisionandagoodunderstandingofthisnoiseisvitaltoanypotentialimprovement. HerewepresentastudyoftheSuperWASP detectormaps,highlightingsomekeyfeaturesandinvestigatingtheircauses.

WhitherUK-LedGround-BasedSubmmAstronomy?

DavidClements (ImperialCollege)

TheUK hasagrandtraditioninground-basedsubmmastronomy, withahugelysuccessfulpastandwithgreatpotentialforthenextfewyearsthankstoSCUBA2. Beyondthistimescale, though,thereisnothingplannedwithclearUK leadership.I willreviewthepastandpresentandlookattherangeofpossibleopportunitiesforthisfieldinthefuture. Thispresentationisthenextstageinaprocessofcommunityconsultationonfacilitydevelopmentsforthefutureofthisfield.

JCMT andUKIRT:GoodNewsandBadNewsGaryDavis (JointAstronomyCentre)

ThetwoUK telescopesonMaunaKeahavehadcontrastingfortunesinthepastyear. UKIRT wasidentifiedfor"managedwithdrawal"bySTFC andIwillreportontheimplementationofthisandontheimplicationsforUKIDSS andotherongoing

programmes. TheJCMT,ontheotherhand, iscurrentlyinthemidstofacampaignofearlysciencewiththerevolutionarySCUBA-2instrumentandI willreportontheoutcomesofthiscampaign, thenear-termplansfortheJCMTLegacySurveyandthelong-termprospectsfortheobservatory.

e-MERLINSimonGarrington (UniversityofManchester)

e-MERLIN willprovide10-150milliarcsecondresolutionimagingatcentimetrewavelengthsandmicroJanskysensitivity. Thesecapabilitiesarevitalforresolvingkpc-scalestar-formingregionsandAGN indistantgalaxiesandAU-scaleprocessesofstar-formationinourGalaxy.Theenhancedsensitivityisbeingachievedwithnewbroad-bandreceiversanddedicatedopticalfibreconnectionstoanewcorrelator. Theinstrumentisbeingcommissionednowandsomeofthefirstresultswillbediscussed.

TheLiverpoolTelescope: ObservationswiththeSTILT (SmallTelescopesInstalledatLT) widefield

instrumentsNeilMawson (AstrophysicsResearchInstitute)

with Iain Steele

STILT isasetofthreewideimagingsetupsthathavetheabilitytoobservethousandsofobjectsinjustasingleimage. Thecurrentsetupincludes: anallskycamera, SkycamA,whichiscapableofimagingto6thmagnitudewhichshowsitiscapableofdetectingsomebrighttransientevents.A 20degreefieldofviewcamera, SkycamT,whichwithitswidefieldandtheabilitytoimageto∼ 12thmagnitudecanobservearound5000starsinasingleimageanda1degreefieldofviewtelescope, SkycamZ,whichiscapableofreaching18thmagnitude. SkycamZ alongwithSkycamT isattachedtothemainbodyoftheLiverpoolTelescopesobenefitsfromthepointingandtrackingabilityoftheLT.Allthreesetupscarryout10secondexposureseveryminute, soprovideconsiderableamountsofdatapernight. Theinstrumentshavebeenrunningforayearnowsothereisalsoanarchiveofunprocesseddatawhichcouldcontaindataonpasttransientevents. Theaimistocreateadatapipeline, whichwillautomaticallyreducethedataandcataloguetheobjectsineachimage. Thencrosscheckwithacurrentdatabaseandcreateanalertforanydetectedobjectwhichthesystembelievestobeofstellaroriginandpreviouslyuncatalogued. SofartheSTILT systemisalreadycontributingtotheanalysisofbothaGRB andanova.

EarlyresultsfromSCUBA2DavidNutter (CardiffUniversity)

Inthistalk, I willhighlightsomeoftheearlyresultsfromtheinitial'sharedrisks'observingperiodofSCUBA2ontheJCMT.InparticularI willshowdatafromtheJCMT GouldBeltSurveyofnearbystar-formingregions, anddetailhowthesedatawillbeusedtoimproveourunderstandingofthestar-formationprocess. Thequestionsthatweseektoanswerwiththesedataincludetherelationshipbetweenthemassfunctionofpre-stellarcoresatthelowestmasses, andtherelativelifetimesofthedifferentevolutionarystagesofstarformation. Iwillalsousesomefar-infrareddatafromtheAkarisatellitetodemonstratewhySCUBA2dataisessentialtocomplementthedatafromtheHerschelsatellite, andwhythelongwavelengthprovidedbySCUBA2, togetherwithshorterwavelengthdatafromHerschelwillbreakthe

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degeneracybetweentemperatureandcolumndensity.

ALMA:statusreportandfirstscienceJohnRicher (Cambridge)with G Fuller, and

T Muxlow

ALMA isnowthelargestworkingsubmillimetreinterferometerintheworld: inDecember2009, itsfirstthree12-mantennasoperatedtogether, andphaseclosurewasachieved. Antennasandreceiverscontinuetoarriveandoverthenext3yearsALMA willgrowintoa66-elementarray.Thefirstcallforscienceproposalsislessthan12monthsawayinthecurrentschedule, andfirstsciencedatashouldbeavailableinlate2011. ThistalkwillsummarisethestateofALMAconstruction, andpresenttheexcitingscientificopportunitiesthatALMA willsoonenable.

HerschelandSPICA:pushingthefrontiersintothecoolcosmos

DimitraRigopoulou (STFC RAL/Oxford)

BuildingontheheritageofthesuccessfulHerschelmissionwillbeSPICA,ajointJAXA/ESA mission.ThisrepresentsamajorstepintheexplorationoftheDustyUniverseinthenextdecade. SPICA willpushthefrontiersonthephysicsofdustandtheinterstellarmediumfromplanetstothedistantUniversewithunprecedentedsensitivity- thankstoitbeingacryo-cooledmission. I willreviewthemajorscientificdriversofthemissionfocusinginparticularonsciencethatwillbecarriedoutwithSAFARI,theEuropean-ledfouriertransformspectrograph.

UpdateontheKMOS SpectrographforESO VLTRaySharples (UniversityofDurham)

KMOS isamulti-objectnear-infraredintegralfieldspectrometerunderconstructionbyaconsortiumofUK andGermaninstitutesfortheESO VLT.KMOS willbethefirstUK-ledfacilityclassinstrumentontheVLT andiscurrentlyinthefinalassembly, integration&testphase. ThistalkwillreviewthescientificpotentialofKMOS andshowtheresultsfromrecentprogressinthesubsystemmanufactureandtest.

P06TheMeerKAT DeepContinuumSurvey

MattJarvis (UniversityofHertfordshire)withKurtvander Heyden

I willpresentthecaseforalargecontinuumsurveytobeundertakenwiththeSouthAfricanSKA precursortelescope, MeerKAT.Scienceaimscovertheevolutionofstar-forminggalaxiesandAGN,cosmologyandlarge-scalestructureandtracingthemagneticfieldsintheUniverse.

EarlyresultsfromthecommissioningofLOFARJohnMcKean (ASTRON) with George Heald, and

LOFAR imagingcommissioningteam

TheLowFrequencyArray(LOFAR) willoperatebetween10and240MHz, andwillobservethelowfrequencyUniversetoanunprecedentedsensitivityandangularresolution. ThemainsciencegoalsofLOFAR aretoi)carryoutdeepextragalacticsurveys, ii)probetheepochofreionization, iii)studycosmicmagnetism, iv)investigatethetransientsky, v)studysolarphysics

andvi)observeultrahighenergycosmicrays.LOFAR willalsoprovideanimportanttestbedforthetechnologies(hardwareandsoftware)thatwillbeusedfortheSKA.

TheconstructionofLOFAR iswellunderway, withoverhalfoftheDutchstationsandthreeinternationalstationsroutinelyperformingbothsingle-stationandinterferometricobservationsoverthefrequencyrangethatLOFAR isanticipatedtooperateat. Here, I summarizethecapabilitiesofLOFAR andreportonsomeoftheearlycommissioningresults, concentratingonthewide-fieldimagingoftestfieldsaround3C 196and3C61.1between30-78MHzand120-168MHz.

RadioWeakGravitationalLensingwithVLA andMERLIN

PrinaPatel (InstitueofCosmology&Gravitation)with D.J. Bacon, R.J. Beswick, T.W.B. Muxlow, and

B. Hoyle

WecarryoutanexploratoryweakgravitationallensinganalysisonacombinedVLA andMERLINradiodataset: adeep(3.3micro-Jyperbeamrmsnoise)1.4GHzimageoftheHubbleDeepFieldNorth. I measuretheshearestimatordistributionatthisradiosensitivityforthefirsttime, findingasimilardistributiontothatofopticalshearestimatorsforHST ACS datainthisfield. Iexaminetheresidualsystematicsinshearestimationfortheradiodata, andgivecosmologicalconstraintsfromradio-opticalshearcross-correlationfunctions. I shallemphasizetheutilityofcross-correlatingshearestimatorsfromradioandopticaldatainordertoreducetheimpactofsystematics. UnexpectedlyI findnoevidenceofcorrelationbetweenopticalandradiointrinsicellipticitiesofmatchedobjects; thisresultimprovesthepropertiesofoptical-radiolensingcross-correlations. I exploretheellipticitydistributionoftheradiocounter- partstoopticalsourcesstatistically, confirmingthelackofcorrelation; asaresultI suggestaconnectedstatisticalapproachtoradioshearmeasurements.

A SETI pilotprogrammewithLOFARAlanPenny (U StAndrews)with M. Garrett

(ASTRON), M. Wise(ASTRON), R. Nichol(UPortsmouth), R. Fender(U Southampton), andH. Falcke(RadboudUniversiteitNijmegen)

TheLOFAR commissioningplanincludesapilotprogrammetoinvestigatetheuseofLOFAR forSETI observations. MostradioSETI searcheshavebeeninthe1-2GHzrange, andtheadventofLOFAR permitsdeepsearchesintherelativelyunexplored80-240MHzrange.

A fewnearbystarswillbesearchedfortheverynarrowbandemissionassociatedwithartificialsources, andthesensitivityofLOFAR anditsabilitytorejectterrestrialsourceswillbeinvestigated.Thisinvestigationwillhaveimplicationsforlow-frequencySETI workwithSKA.

PathwaytotheSKASteveRawlings (UniversityofOxford)

I willdiscussthesciencecasesforthevariouspathfinderandprecursortelescopesonthepathwaytotheSKA illustratinghowtheyinformonkeySKA science. TheseideaswillbeextendedtomapscienceoutputontothephasedconstructionoftheSKA itself.

P07Herschel: statusandin-orbitperformance

MattGriffin (CardiffUniversity)with ESA, SPIREconsortium, PACS consortium, and HIFI

consortium

ESA’sHerschelSpaceObservatorywaslaunchedinMay2009. Itisthefirstlarge-apertureFIR/submmspacemission, andthefirsttoextendbeyond200micronswavelength. Itcarriesa3.5-mdiametertelescope(thelargestastronomicaltelescopeyetflown), passivelycooledtoaround85K,andthreecryogenicallycooledscientificinstruments. PACS hasafarinfraredcameraoperatingat70, 100and160microns, andanimaginggratingspectrometercovering55–210microns. SPIRE hasathree-bandsubmillimetrecameraoperatingsimultaneouslyat250, 350and500microns, andanimagingFouriertransformspectrometercovering194–670microns. HIFI isaseven-channelsingle-pixelhigh-resolutionheterodynespectrometercoveringmostofthesubmillimetreregion. Thissuiteofinstrumentsallowsastronomerstocarryoutsensitiveimagingandspectroscopyoveradecadeinwavelength.HerschelhasbeenplacedinanorbitaroundtheSun-EarthL2point(aposition1.5millionkmdistantfromEarth, ontheanti-sunwardside), andwillhaveanoperationallifetimeofatleastthreeyears. Afterseveralmonthsofcommissioningandperformanceverification, thespacecraftandallthreeinstrumentsareperformingextremelywell.Manysuccessfulsciencedemonstrationobservationshavebeencarriedoutandroutineobservationsarenowunderway. I willdescribethemainfeaturesoftheobservatoryandtheperformanceandscientificcapabilitiesoftheinstruments.

SWIRE 70micronselectedGalaxies: FollowupandLuminosityFunction

HarsitPatel (ImperialCollegeLondon)withD.L. Clements

WepresenttheopticalandfarIR propertiesof70micronselectedgalaxiesfromtheSWIRE XMMLSSandLockmanfields. Wehaveobtainedspectroscopicredshiftsfor300newsourcesdownto70micronfluxlimitof9mJyand R < 22. Theredshiftdistributionpeaksat ∼ 0.3 andhasahighredshifttailouttoz=3.5. WeperformemissionlinediagnosticsforsourceswhereHα, Hβ, [NII]and[SII] emissionlinesareavailabletodeterminetheirpowersource. WefitsingletemperaturedustSEDs, Fν = Aβ

νB(ν, T ), to70micronsourceswith160micronphotometrytoestimatedusttemperaturesandmasses. Assumingadustemissivityindexof1.3wefindtemperaturesintherange ∼ 30 –50K anddustmassesintherange106–109 M⊙whichisconsistentwithresultsobtainedforSLUGS galaxies. Increasing βto2resultsinslightlycoldertemperatures, whichsuggesttheneedtoaccuratelydeterminetheshapeoftheRayleigh-JeanstailofthedustSEDandmoreimportantlytounderstandtheroleofcolderdust. TherecentlylaunchedHerschelsatellitewillshedlightontheseissues. WethenbuildfullSEDsforeachsourceusingthemultiwavelengthdatafromopticaltofar-IR.WefindinoursamplesourceswithIR luminositiesinrange108–1013 L⊙. TheSED fitsarethenusedtoconstructthelocal(z < 0.5)70micronluminosityfunctionandcompareourresultswiththeIRAS 60micronluminosityfunction.

50 P05–P07

FirstresultsfromtheDEBRIS surveyNeilPhillips (InstituteforAstronomy, UniversityofEdinburgh)with Jane Greaves, Brenda Matthews,Bruce Sibthorpe, Grant Kennedy, Laura Churcher,Amaya Moro-Martin, Mark Wyatt, and DEBRIS

consortium

TheDEBRIS surveyistargetingalargesampleofnearbymain-sequencestarsystems, exploitingthewavelengthcoverage, spacialresolutionandsensitivityofHerscheltodiscoverandcharacterisecooldebrisdiscs. HerewepresentfirstresultsofPACS 110and170micronsimagingoffivenearbyA andF typestarswithsignificantdustemission(βLeo, βUMa, ηCrv, ζTuc, ζDor). TheseobservationsarecomparedwithSpitzer/MIPS andJCMT/SCUBA imagesatshorterandlongerwavelengthsrespectively.

TheHerschel-ATLAS:A firstlookEmmaRigby (UniversityofNottingham)with H-

ATLAS team

TheHerschel-ATLAS isthelargestoftheHerschelSpaceObservatory'sopen-timekeyprogrammes.Itisalargeareaextragalacticsurveyprovidingsimultaneousfivebandphotometryacrossawavelengthrangeof110-500microns. TheareacoveredisfourtimesgreaterthanalltheotherHerschelextragalacticsurveyscombined, givingatotalcoverageof550squaredegrees. I willdescribethesurvey, andtheplannedscienceprogrammesassociatedwithit, andpresentthefirstresultsfromthesciencedemonstrationphaseobservations.

InitialresultsfromHerMES:theHerschelMulti-tieredExtragalacticSurvey

AnthonySmith (UniversityofSussex)withHerMES Consortium

HerMES,theHerschelMulti-tieredExtragalacticSurvey, isthelargest(900hour)guaranteed-timekeyprojectonHerschel, designedtocharacterizefar-infraredandsubmillimetregalaxypopulationsoverbroadrangesofredshift, luminosity, andenvironment. Targetfieldsrangeinsizeanddepthfromfractionsofasquaredegree, withdepthsbelowthesubmillimetreconfusionlimitforcharacterizingthegalaxiesthatcontributethebulkofthefar-infraredandsubmillimetreextragalacticbackground, totensofsquaredegreesforprobinglarge-scalestructureandtherelationoffar-infraredgalaxiestodarkmatter. A subsetofinitialresultsfromtheScienceDemonstrationPhasewillbesummarized, indicatingthehigh-redshiftscienceattainablewithHerschel. Areasofscienceinclude: measurementsofsourceconfusionnoiselevelsasafunctionofwavelength, galaxynumbercountsviadetectionstatisticsandfluctuationanalyses, galaxycolours, preliminaryspectralenergydistributionsandluminosityfunctionsforsamplesofgalaxies, andearlyimplicationsforgalaxymodels.

TheHerschelVirgoClusterSurvey(HeViCS)MatthewSmith (CardiffUniversity)with HeViCS

Consortium

TheHerschelVirgoClusterSurvey(HeViCS) isanopentimekeyprojecttoobserve64squaredegreesofthenearbyVirgoCluster. Theclusterwillbeobservedinparallelmodeprovidingdataat100, 160, 250, 350and500microns; whichcanbecombinedwithawealthofdataatotherwavelengths. I willdescribethemotivationforthesurvey, thescientificobjectivesandsomeofourfirstresultsfromsciencedemonstrationdata.

EarlyHerschelResultsonStarFormationDerekWard-Thompson (CardiffUniversity)with

J.M. Kirk, D. Stamatellos, and L. Wilcock

EarlyresultsfromHerschelarepresentedofanumberofstar-formingregions. Imagingat5wavebandsfrom70to500micronsallowopticaldepthandtemperaturemapstobemade. Coresonthevergeofformingstarsareidentifiedandmodelled. Someofthesearestarlesscores, someareprestellarandsomeareso-calledinfrareddarkclouds(IRDCs). FTS spectroscopyalsoallowsthegastobestudiedalongwiththedust. Typicalspectrashowthe12CO and13CO laddersoflines, aswellasCI.Weuseamonte-carlomodeltoobtainthephysicalparameterswithinIRDCsforthefirsttime. Theimplicationsfortheformationofhigh-massstarsarediscussed.

SPIRE FTS spectraofthreecarbon-richevolvedobjects

RogerWesson (UniversityCollegeLondon)withJ. Cernicharo, M. Matsuura, M. Barlow, L. Decin,

E. Polehampton, and MESS consortium

Lowtointermediatemassstarslosemostoftheirmassduringtheirfinalstagesofevolution, intheformofcool, lowvelocitywinds. Thismasslossisthedominantcontributortotheenrichmentoftheinterstellarmedium. Thepost-AGB objectsAFGL618andAFGL 2688, andtheplanetarynebulaNGC 7027areamongthebest-studiedcarbon-richevolvedsources, andISO observationsshowedthemtohaverichinfraredspectra. WehaveobtainedhighsignaltonoiseSPIRE FTSspectraofthesethreeobjects, coveringwavelengthsfrom200-670microns, apreviouslyunexploredregionofthespectrum. A largenumberofatomicandmolecularlinesfromawiderangeofspeciesaredetected; wepresentthesenewspectraandpreliminaryanalyses

P08Giantplanetmagnetospheres: JupiterandSaturnChrisArridge (UniversityCollegeLondon–MSSL)

ThemagnetospheresofJupiterandSaturnarethelargestandmoststudiednon-terrestrialmagnetospheresintheSolarSystem. Thevastsizeofthesestructuresispartlyduetostronginternaldynamosandlargeplanetarymagneticmoments,andpartlyduetotheirlocationintheheliospherewherethedynamicpressureofthesolarwindislowerthanthatneartheterrestrialplanets. Insidethejovianandkronianmagnetospheres, largeneutraltoriiformfromneutralssputteredandejectedfromthesurfacesoficyandvolcanicsatellites. Theseneutraltoriibecomeionised,producingplasmatorii. Thisplasmaisthensubjecttoaradialdiffusionprocess, knownasinterchange, whichspreadstheplasmathroughoutthemagnetosphere. Strongcentrifugalforcesassociatedwiththerapidlyrotatingplasmaconcentratethismaterialintoadisc. Outwardtransportandcouplingbetweentheplanet'sionosphereandequatorialmagnetospherealsoresultsinangularmomentumtransportbetweentheplanetandthemagnetosphericplasma. Inthistalktheconfigurationandequilibriumofthejovianandsaturnianmagnetosphereswillbereviewedandwillfocuson: magnetosphericstressbalance, magnetosphere-ionospherecouplingandthegenerationofplanetaryaurorae. Weshalldiscusstheeffectsofdipoletiltandsolarwind

forcingandhowtheseprocesses"break"theidealisednorth-southmagnetosphericsymmetry.Thetalkwillconcludewithcommentsonthecomparisonbetweengiantplanetandcooldwarfmagnetospheres.

Dynamicspectraofindividualradiopulsesinanultracooldwarf

GreggHallinan (UC Berkeley)

A numberofverylowmassstarsandbrowndwarfshavebeendetectedproducingperiodicpulsesofradioemission, whichhaveledtothesesourcesbeingdubbed"ultracooldwarfpulsars".OurbestevidencetodatesuggeststhisradioemissionisofthesamenatureasthatdetectedatkHzandMHzfrequenciesfromthemagnetizedplanetsinoursolarsystem, butrequiringmuchmorepowerfulkilogaussmagneticfields. Morerecently, periodicsignalsofthesameperiodasthosedetectedintheradiohavebeenfoundinopticalandinfraredphotometricandspectroscopicdataforanumberoftheseultracooldwarfpulsars. I willdiscusstheresultsofarecentArecibocampaignthatprovidesbroadbanddynamicspectraofindividualradiopulsesfromtheseobjectsaswellasamultifrequencyobservationinvestigatingtherelationshipbetweentheradiopulsesandthemysteriousperiodicsignalsdetectedinopticalandinfrareddata.

PhysicalParametersofUltracoolDwarfs: TheYoungandTheOld

RobertKing (UniversityofExeter)withMarkJ. McCaughrean, Jenny Patience,

Catia Cardoso, RobertDe Rosa, Derek Homeier,and France Allard

I willpresentourcomprehensivestudyofthephysicalpropertiestheoldfieldbrowndwarfbinary εIndiBa, Bb, thenearestbrowndwarfstotheSun, includingresultsfromhighangularresolutionoptical, near-infrared, andthermal-infraredimagingandmedium-resolution(uptoR∼ 5000)spectroscopyoftheindividualcomponents, andournear-completeastrometricmonitoringtodeterminethedynamicalsystemandindividualmassesofthesetwoT dwarfs. I willthendetailtheobservationsandinterpretationoftheyoung, low-massobject2M1207b, ayoungLdwarfwithanestimatedmassof ∼ 10MJup, butananomalouslylowluminosity. Thisobjectwillserveasakeycomparisonforupcomingnear-infraredspectroscopyofplanetsimagedaroundstellarhosts.

Finally, I willbrieflydiscusstheproblemsassociatedwithinferringphysicalpropertiesofultracooldwarfsfromlimiteddatasetsandthepossibilitiesforusinghighresolutionspectroscopicobservationsofultracoolbinariestoextractestimatesofthemetallicityfromsingleobjectsandso, inthelongerterm, investigateanydifferenceinheavymetalenrichmentwhichmayindicateformationthroughcoreaccretion.

Numericalsimulationoftheelectron-cyclotronmaserinstabilityinthemagnetospheresofbrown

dwarfsAlexeyKuznetsov (ArmaghObservatory)with

Gerry Doyle

Recently, anumberofbrowndwarfshavebeenfoundtobebrightradiosources. Theirradioemissionhashighbrightnesstemperature, highpolarizationdegree, andnarrowdirectivity. Theemissionisproducedmostlikelyduetotheelectron-cyclotronmaserinstabilityinaway

P07–P08 51

similartotheauroralradioemissionofthemagnetizedplanetsoftheSolarsystem. Inthiswork, wesimulatenumericallygenerationofradioemissioninmagnetospheresofbrowndwarfs. A2D codehasbeendevelopedtoinvestigatetheco-evolutionofanelectrondistributionandadistributionofmagnetoionicplasmawaves. Theinfluencesofaconvergingmagneticfieldandafield-alignedelectricfieldareconsidered, too. Thesimulationparameterswerechosenbasingonthemeasurementsintheterrestrialmagnetosphereandscaledtofittheexpectedconditionsatbrowndwarfs. Wefoundthatthedownward-directedaccelerationofelectronsbyfield-alignedelectricfieldtogetherwiththereflectionofparticlesfrommagneticmirrorresultinformationofthe"horseshoe"-likedistributions. Suchdistributionsareunstablewithrespecttoexcitationofdifferentmagnetoionicmodes, buttheZ-modeisdominant.AmplificationoftheZ-modewavesandtheelectrondiffusiononthemresultinarapidsaturationoftheelectron-cyclotronmaser, andthenthegrowthratesofallmodesdecreasesignificantly. Thefastordinaryandextraordinarymodesareneveramplifieduptothesaturationlevel. Ontheotherhand, thecontinuingactionofthefield-alignedelectricfieldandconvergingmagneticfieldpreventsthewave-particlesystemfromreachingacompletelysaturatedstate. Inparticular, thesefactorsareabletokeepthegrowthrateofthefastextraordinarymodeatthelevelsufficienttoproduceanintenseradioemission. Weusethesimulationresultstointerprettheobservations, andtoestimatetheparametersoftheemissionsources.

ThePeculiarbehaviourofRadioEmissioninFullyConvectiveStars

PaulineLang (UniversityofStAndrews)withMoira Jardine

LowMassStarshavebecomethesubjectofintensestudyasthesearchforexoplanetsbecomesmoreadvanced. M Dwarfsareofparticularinteresttousastheycanbethoughtofasthe'boundary'starsbetweenthesolar-typestarswithradiativecoresandconvectiveenvelopesandtheUltraCoolDwarfswhicharefullyconvective. InmainsequencestarsthereisadirectcorrelationbetweenX-rayluminosityandRadioluminosity.However, whenweentertherealmofthelowmassstarsthisrelationshipbreaksdown. Acrossthefully-convectiveboundarytheX-rayluminositychangeslittle, buttheradioemissionincreases; infactthelessmassivethestarthegreaterthiseffectbecomes. Workingundertheassumptionthattheradioemissioncouldbebeingproducedinanauroralring-likestructurenearthemagneticpoleofthestar, weaimtoreproducetheradiolightcurveseeninstarssuchasV374Peg.

UltraspecObservationsofTVLM 513-46546StuartLittlefair (UniversityofSheffield)

TVLM 513-46546isthebeststudiedoftheultracooldwarfpulsars; verylowmassstarswhichshowpulsedradioemissionontherotationalperiodofthestar. TheopticalvariabilityofTVLM513-46546presentsapuzzle. Itshowsperiodicvariabilityontherotationperiod, butmulti-bandobservationssuggesttheopticalvariabilityisdominatedbypatchydustcloudsinapredominantlyneutralatmosphere. Thisissurprisinginthecontextoftheradioemission.

HerewepresenttimeresolvedspectrophotometryofTVLM 513-46546usingtheelectronmultiplyingCCD,Ultraspec, takenaspartofa

multi-wavelengthcampaign. ThisdatasetallowstherelationshipbetweentheopticalvariabilityandtheHalphalinefluxtobeinvestigated,sheddingnewlightontheopticalvariabilityofTVLM 513-46546.

StructureanddynamicsoftheboundaryofSaturn'smagnetosphere

AdamMasters (UniversityCollegeLondon–MSSL) with N. Achilleos, A.J. Coates, and

M.K. Dougherty.

TheCassinispacecraft’sorbitaltourofSaturnallowsustostudytheboundaryofagiant,corotation-dominatedmagnetosphereintheoutersolarsystem. ProcessesoperateatthisinterfacebetweenthesolarwindandSaturn’smagnetospherethatleadtothetransportofmass,momentumandenergyintothesystem. TheresultsofasurveyofthecrossingsoftheboundaryregionmadebytheCassinispacecraftarepresented. Theorientationofthemagnetopausecurrentlayerisdeterminedforthemajorityofthecrossings. Ananalysisoftheboundarynormalssuggeststhatthecrossingsmadeduringanumberofspacecraftorbitsweretheresultofwaveactivityonthemagnetopausesurface. Thelow-latitudeinternalboundarylayerischaracterised. Variationsintheboundarylayerandthedependenceofthepropertiesofthelayerondifferentparametersareinvestigated. Thewiderrelevanceoftheseresultsformagnetosphericscienceisdiscussed.

VariationofSaturn'sUV aurorawithSKR phaseJonathanNichols (UniversityofLeicester)with

B. Cecconi, J.T. Clarke, S.W.H. Cowley,J.-C. Gerard, A. Grocott, D. Grodent, L. Lamy, and

P. Zarka

Itiswellknownthatvariouskronianmagnetosphericphenomenaexhibitoscillationsneartheplanetaryrotationperiod. However, theemittedUV auroralpowerhasnotbeenshowntovaryattheSKR period. Weuseanempirically-determinedSKR phasetoorderthe'quiettime'totalemittedUV auroralpowerasobservedbytheHubbleSpaceTelescopein2005, 2007, 2008and2009. OurresultssuggestthattheUV powerisapparentlydependentonSKR phase, althoughthepowervariationisonlybyfactorsoforder ∼ 2,ratherthantheordersofmagnitudeobservedintheSKR.Wealsoshowthatthevariationoriginatesfromthemorninghalfoftheoval, consistentwithpreviousobservationsofthesourceoftheSKR.

Sourceofperiodicradioemission; lessonsfromSaturn

DavidSouthwood (ESA) with M.G. Kivelson

ThepulsingradiosignalsfromSaturn(Saturnkilometricradiation, SKR),yieldsomeinterestinglessonsforboththeproblemofidentifyingtheultimatesourceoftheradiosignalbutalsoonwhatmaybededucedfromperiodicradioemissioningeneral. Commonlyithasbeenthoughtthatperiodicradioemission, becauselinkedtothemagneticfieldyieldsdirectinformationonthedeeprotationofanobject.WhatisknownfromSaturndrawsthisassumptionintodoubt. WereviewwhatisknowntherelationbetweentheSaturnemissionandtheplanetarymagnetosphericmagneticfieldaftersixyearsofCassinispacecraftorbitaldata. TheSKR isgeneratedastheby-productofaninternalinteractioninthemagnetosphere. Theperiodicsignalisinpracticepulsedandyetlinkedtoarotatingmagneticstructure. Theprimaryinteractionisaresultofthemodulationoffield-

alignedcurrentsgeneratedbetweentheoutermagnetosphericfieldwhereitisstressedbythesolarwindandarotating“cam”magneticfieldstructurewhichisthedominantfieldperturbationintheinnerandmiddlemagnetosphere.

InfluenceofupstreamsolarwindconditionsonatmosphericflowsatJupiter

JaphethYates (UniversityCollegeLondon)withNicholas Achilleos, and P. Guio

ThecouplingofJupiter'smagnetosphereandionosphereplaysavitalroleincreatingitsauroralemissions. ThestrengthoftheseemissionsissomewhatdependentontherelativerotationalflowswithinJupiter'sthermosphereandthemagnetodisc. Usinganazimuthallysymmetricglobalcirculationmodel, wewereabletosimulatehowup-streamsolarwindconditionsaffectatmosphericflows; herewepresentthesepreliminaryestimates. Wecalculatedmagneticfieldprofilesrepresentingcompressedandexpandedmagnetospheres, andtheseprofileswerethenusedtogainfurtherinsightonthemagneticconfigurationandcouplingofthemagnetospherewiththeionosphereandhowthiseffectsglobalwindsandenergyinputswithinJupiter'sthermosphere.

Mappingradioemitting-regiononlow-massstarsandbrowndwarfs

ShenghuaYu (ArmaghObservatory)withJ.G. Doyle, G. Hallinan, A.L. MacKinnon, and

A.E. Antonova

A numberofrecentradioobservationsindicatemagneticactivityoperatedbydynamotheorywouldbecommonphenomenononultracooldwarfs(UCDs, spectralclasseslaterthanM7).Currently ∼ 11 radioactiveUCDsareshowingveryhighbrightnesstemperatureandhighly(upto100%)circularpolarization, including3withstrongperiodicradiobeams. Thenatureoftheemissioncouldbeinterpretedbyaneffectiveamplificationmechanismofthehigh-frequencyelectromagneticwaves- theelectroncyclotronmaser(ECM) instability. Wehaveperformedone-dimensionalparticlesimulationtoinvestigateresponseofweaklyrelativisticelectronbeamstoamagnetic-field-alignedelectricfieldinducedbyatime-varyingexternalcurrentsource. Wefoundrelativisticelectronbeamscouldresultinstrongerinstabilitythannonrelativisticbeams. Bythesimulation, weareabletodeterminethesizeandheightofradioemitting-region, electrondensity,timescaleoftheinstabilityandevensurfacemagneticfieldofUCDs.

P09Determinationofthephotometriccalibrationandlarge-scaleflatfieldoftheSTEREO Heliospheric

Imagers: I.HI-1DanielleBewsher (JeremiahHorrocksInstitute,UCLan)with D.S. Brown, C.J. Eyles, B.J. Kellett,

G.J. White, and B. Swinyard

Theaimofthispaperistocalculateanaccuratelarge-scaleflatfieldfortheSTEREO HI-1instruments. ThisisdonebyanalysingthevariationinintensityofstarsinthebackgroundstarfieldastheypassacrosstheCCD.Inordertousethebackgroundstarfield, aphotometriccalibrationisperformedwhichdefinesaHImagnitudescaleandaconversionbetweenthis

52 P08–P09

scaleandmeasuredintensity. Thephotometriccalibrationusesstellarspectrafoldedthroughtheinstrumentresponsetomakeinitialintensitypredictions. However, asecondarypredictionmethodbasedonthephotometriccalibration,whichblendstheR-, V- andB-magnitudesofastar, isderivedforstarswithnospectralinformation. Inaddition, asolarspectrumfoldedthroughtheinstrumentresponseisusedtodetermineconversionfactorstoconvertfromHIintensityunitsintomeansolarbrightness, S10andSI units, fordiffuseorextendedsources.

TheRosettaPlasmaConsortiumChrisCarr (ImperialCollegeLondon)with

Elizabeth Lucek

TheRosettamissionisoneoftheoriginal‘cornerstone’missionsofESA’sHorizons2000scienceprogramme. Thespacecraftwaslaunchedin2004, willrendezvouswiththecomet67PChuryumov-Gerasimenkoin2014, followthecometfromdeep-spacethroughtoperihelion, andplacealandercraft(Philae)onitssurface.Consequently, Rosettawillallowbothremotesensingandinsitumeasurementssimultaneously.Cometscontainthemostpristine, least-processedmaterialinoursolarsystem. Thereareprobablyevenpre-solargrainspreservedinsidethesebodies. TheaimofRosettaisnothinglessthantounderstandtheoriginsofthesolarsystem. Rosettaappealstotwodistinctcommunities: theplanetaryandsolarsystemscientistswhowillinterpretcometsasthebuildingblocksofthesolarsystem,andthespacescientistswhoareconcernedwiththegas/dust/plasmainteractionwiththesolarwind. Forboth, thecometisanaturallaboratorywhichwouldbeimpossibletore-createontheground. RosettahastheopportunitytobringthesestrongUK communitiestogether, furthermorethereisplentytointerestastronomerstoo. TheRosettaPlasmaConsortium(RPC) isasuiteofinstrumentationontheorbiterspacecraftdedicatedtounderstandingtheevolutionofthecomet/solar-windinteractionasafunctionofheliocentricdistance(andhencecometaryactivity). InthisposterweoutlinethescientificpossibilitiesoftheRPC meaurements. Wedescribethecapabilitiesoftheinstrumentsuiteandtheexpectedenvironmentinwhichtheywilloperate.

EuropaJupiterSystemMissionMicheleDougherty (ImperialCollegeLondon)

TheEuropaJupiterSystemMission(EJSM) isaninternationalmissiontotheJupitersystemwithjointparticipationfromESA andNASA.ItconsistsoftwoprimaryflightelementsoperatingintheJoviansystem: theESA-ledJupiterGanymedeOrbiter(JGO) andtheNASA-ledJupiterEuropaOrbiter(JEO).JGO andJEO willexecuteanextendedchoreographedexplorationoftheJupiterSystembeforesettlingintoorbitaroundGanymedeandEuropa, respectively. TheoverarchinggoalofEJSM isthestudyoftheemergenceofhabitableworldsaroundgasgiants. JGO andJEO willcarrycomplementaryinstrumentstoachievethefollowingscienceobjectives: characterizeGanymedeandEuropaasplanetaryobjectsandpotentialhabitats, studyGanymede, Europa,CallistoandIointhebroadercontextofthesystemofGalileansatellitesandfocusonJupiterscienceincludingtheplanet, itsatmosphereandthemagnetosphereasacoupledsystem.

SOHO CoronalDiagnosticSpectrometerAndrzejFludra (STFC RutherfordAppleton

Laboratory)with Andrzej Fludra(STFC RutherfordAppletonLaboratory)

TheSolarandHeliosphericObservatory(SOHO),launchedinDecember1995, hasbeeninoperationforover14years. TheCoronalDiagnosticSpectrometer(CDS) isaUK-ledinstrumentonboardSOHO,operatedbyateamfromtheRutherfordAppletonLaboratory. TheCDS facilityhasbeenusedextensivelybyalargeusercommunity, including15UK researchgroupsandover60groupsworld-wide, andsciencestudiesfill24hourseachday. CDS continuestobeusedforallaspectsofsolaratmosphericresearchthatcanbestudiedfromEUV spectra,participatinginregularobservingcampaignswithHinodeandSTEREO spacecraft. Recenthighlightsincludenewactiveregionloopsanalysis, newresultsonexplosiveandgentlechromosphericevaporationduringflares, spatiallyresolvedanalysisofactiveregionheatinginthetransitionregionemission, andjointobservationsofHeliumlinesbythreespectrometers(CDS,SUMER andEIS) thatrevisethelong-standingproblemofenhancedHeliumlineintensities. CDS remainstheonlyspectrometerobservingstrongspectrallinesfromseveralspecies, includingionsofFe, Si,Al, Mg, Ca, Ne, N,O,andHe. Bright, unblendedlinesatcooler, transitionregiontemperaturesareuniquetoCDS andprovidemeasurementsofDopplervelocitiesofthecoolfilamentmaterialassociatedwithnearlyalleruptionsleadingtoCoronalMassEjections, throughlinesofHeI andO V.CDS willthusbetheonlyavailablesourceofspectroscopiccharacterisationoftheunderlying,coolplasmainvolvedineruptiveeventsandCMEsobservedwiththeSolarDynamicsObservatoryAIA fromApril2010. JointCDS andSDOobservationswillbealsovitalforstudiesofthermalstructureandheatingofloopsinthequietsunandactiveregions, thesolarEUV irradiance,andin-flightcalibrationofthespectralresponseoftheSDO AIA bands.

Scienceopportunitiesforgeospacestudies?MikeHapgood (STFC RutherfordAppleton

Laboratory)

Thenear-Earthspaceenvironmentisanimportanttargetforscientificresearcharoundtheworld. Itsdifferentregions(ionosphere/thermosphere,plasmasphere, radiationbeltsandmagnetosphere)exhibitmanyphysicalprocessesthatchallengeourunderstanding, thatareoftenofpracticalimportanceandthatareexemplarsofprocessesthatoccurinmanyotherastrophysicalenvironments. ThistalkwilloutlineanumberofcurrentandfutureopportunitiestostudytheseregionsandexplorehowUK scientistscanexploitthoseopportunities.

TheSTEREO MissionRichardHarrison (RutherfordAppletonLaboratory)

with C.J. Davs, J.A. Davies, C.J. Eyles, andS. Crothers

WeprovideastatusreportontheNASA STEREOmissionandinparticularontheUK-ledHeliosphericImagerinstruments, includinganupdateofrecentscientificresults.

SuperDARN UK:A newresourcetostudyoftheupperatmosphere

MarkLester (UniversityofLeicester)withG. Chisham, M.P. Freeman, S.E. Milan, J.A. Wild,

and T.K. Yeoman

TheSuperDualAuroralRadarNetwork(SuperDARN) hasprovidedobservationsofthepolar, auroral, andsub-auroralionosphereinbothhemispheresforthelast16years. TheUK hasplayedacentralroleintheinitialdevelopmentofSuperDARN andinitsexpansionthroughtheconstructionandoperationsofradarsatHalleyAntarctica, fundedbyNERC,andinFinlandandIceland, fundedbyPPARC andSTFC.FurthermoretheUK hasbeenoneofthemajorusersofthedatafromthenetwork. WiththemoveofgroundbasedSTP fromSTFC toNERC,thewholeoftheUK'scontributiontoSuperDARN comesundertheremitofNERC.Recently, ajointprogrammebetweentheBritishAntarcticSurvey(BAS) andtheUniversityofLeicesterhasseenthedeploymentofaradarontheFalklandIslandsspecificallytoinvestigatetheupperatmosphereinthatregion.AninitiativebeingdevelopedbyBAS,theUniversityofLeicesterandLancasterUniversitywillprovideanewUK facility, SuperDARN UK,whichwillenabletheUK atmosphericcommunitytohave(i)directaccesstocontinuousregionalsynopticandclimatologicalmeasurementsofwinds, wavesandtidesintheNorthandSouthAtlanticsectorupperatmosphere, andofenergyinputsfromSpace; (ii)opportunitiestoruntheirownupperatmosphereexperimentsononeormoreradars, forupto50%ofthetotaloperationaltime; (iii)immediatehigh-leveldataproductsfromthewiderSuperDARN network; (iv)usersupportforSuperDARN dataanalysissoftwareandexperimentdesign; and(v)trainingopportunitiesforstudentsinradartechnologyandatmosphericscienceexperiments. Inthispresentationwegiveanoverviewofthesystem, thedataproductsavailableandthesciencewhichcanbeachievedwithSuperDARN.

ClusterFGM:currentandfuturescientificopportunities

ElizabethLucek (ImperialCollege)with C.M. Carr

Theuniquefour-point, multi-instrumentmeasurementsmadebytheClusterspacecraftovernearly10yearshavealreadyrevolutionisedourunderstandingofthedynamicsofspaceplasmaphysicsprocesses. However, therecentextensionofthemissionuntiltheend2012, togetherwiththeevolutionofthespacecraftorbittocrossnew,asyetunexploredregionsofthemagnetosphere,promisethatdiscoverieswillcontinuetobemade.TheopportunityforscientificprogressisalsosupportedbytheunprecedentedwealthofhighqualityandhighresolutiondatafromallClusterinstruments, availabletoallscientiststhroughtheESA ClusterActiveArchive. Inthepastfewyearsthesatelliteorbithasevolvednaturally, andmeasurementshavealreadystartedtobemadeintheauroralaccelerationregion. Anotherproductiveareahasbeenincollaborationswiththe5THEMIS spacecraftlaunchedbyNASA.Inthenearfutureadditionalkeysciencetargetswillbemeasurementsofcurrentdisruptioninthetail;samplingthepartialringcurrentanditsconnectionwithmagnetosphericcurrentsystems;measurementoftheradiationbeltsandtheinnerplasmasphere; andconjunctionswithSWARM:3satellitesscheduledforlaunchbyESA in2011tomakecomprehensivemeasurementsofthestrength, directionandevolutionoftheEarth’sfield. Finally, anewinitiativetoopenupCluster

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sciencetothewiderscientificcommunityhasbeenmadebymakingacallforscienceproposalsfor“specialorbits”, allowinginstrumentoperationstobetailoredtoaparticularscientifictarget, Thenewemphasisonmeasurementsoftheinnermagnetospherepresentchallengesforthemagnetometer, asthemagneticfieldmagnitudeexceedsourexpectedoperatingrange. Inthisposterweconsidersomeoftheforthcomingscientificopportunities, andsummarisethestatusofFGM calibrationsanddataavailability.

SolarOrbiter: exploringtheSunandHeliosphereconnection

RichardMarsden (ESA)

UnderstandingtheconnectionsandthecouplingbetweentheSunandtheheliosphereisoffundamentalimportancetoaddressingoneofthemajorscientificquestionsoftheESA CosmicVision2020programme: "HowdoestheSolarSystemwork?"Theheliospherealsorepresentsauniquelyaccessibledomainofspace, wherefundamentalphysicalprocessescommontosolar,astrophysicalandlaboratoryplasmascanbestudiedunderconditionsimpossibletoreproduceonEarth, ortostudyfromastronomicaldistances.TheresultsfrommissionssuchasHelios, Ulysses,Yohkoh, SOHO,TRACE andRHESSI,aswellastherecentlylaunchedHinodeandSTEREOmissions, haveformedthefoundationofourunderstandingofthesolarcorona, thesolarwind,andthethree-dimensionalheliosphere. Eachofthesemissionshadaspecificfocus, beingpartofanoverallstrategyofcoordinatedsolarandheliosphericresearch. However, animportantelementofthisstrategyhasyettobeimplemented.NoneofthesemissionshavebeenabletofullyexploretheinterfaceregionwherethesolarwindisbornandheliosphericstructuresareformedwithsufficientinstrumentationtolinksolarwindstructuresbacktotheirsourceregionsattheSun.ThisistheoverarchinggoalofSolarOrbiter. Withpreviouslyunavailableobservationalcapabilitiesprovidedbythepowerfulcombinationofin-situandremotesensinginstruments, andtheuniqueinner-heliosphericmissiondesignspecificallytailoredforthetask, SolarOrbiterwilladdressthecentralquestionofheliophysics: HowdoestheSuncreateandcontroltheheliosphere? Inthispaper, wewillpresentthedetailedsciencegoalsofthemissionandbrieflyreviewitsstatus.

SolarOrbiter: TheSolarWindAnalyserInvestigation

ChristopherOwen (UniversityCollegeLondon–MSSL) with D.O. Kataria, B.K. Hancock,

A.N. Fazakerley, C. Brockley-Blatt, P. Louarn,S. Livi, and R. Bruno

SolarOrbiterwillexploreinnermostheliospheretounravellinksbetweenactivityinthemagneticfield-dominatedregimeofthesolarcoronaandtheirconsequencesintheparticle-dominatedregimeoftheinterplanetarymedium. TheselinkswillberevealedthroughanalysisofobservationsoftheSunfromacomplementofpowerful, high-resolutionopticalinstruments, togetherwiththosefromstate-of-the-artinstrumentswhichsample, insitu, theproperties, dynamicsandinteractionsofplasma, fieldsandparticlesinthenear-Sunheliosphere. Inaddition, theseplasmaandfieldinstrumentshavehightemporalresolutions, andthusofferuniquepossibilitiesforresolvingplasmakineticprocessesatintrinsicscales.

Inordertoachievethemissionsciencegoals, weneedhigh-cadencemeasurementsof3D velocity

distributionfunctionsofthesolarwindelectron,protonand α−particlespopulations, abundantheavyionssuchasO6+andlowironchargestatessuchasFe9+orFe10+. ThesemeasurementsareamongthosethatwillbemadebytheSolarWindAnalyser(SWA) suiteonSolarOrbiter. Thisinvestigationrequiresmajorinternationalhardwarecollaborations, butisledbytheUK (P.I.institute: UCL/MullardSpaceScienceLaboratory).Inadditiontotheoverallleadershipofthesuite,UCL/MSSL willprovidethebulkofthehardwarefortheElectronAnalyserSystem, oneof3sensorsystemswithinthesuite. TheProton-AlphaSensorandtheHeavyIonSensorareledbypartnersinFranceandtheUSA respectively, whileacentraldataprocessingunit, tobebuiltinItaly, servesall3sensorsandcompletesthesuite.

Inthisposterwebrieflypresentthesciencegoalsrelatedtotheinsituexplorationoftheinnerheliosphereand, inparticular, weaddresstheSWA sensordesignsrequiredtomeetthesegoalsunderSolarOrbiterschallengingmeasurementenvironment.

HinodeUnveilsA NewSunJianSun (UniversityCollegeLondon–MSSL) with

Louise Harra, David Williams, Len Culhane,Lucie Green, and Deb Baker

HinodeisajointJapan/UK/US missionwithESAandNorwegianinvolvement. Usingacombinationofoptical, EUV andX-rayinstrumentationHinodewillstudytheinteractionbetweentheSun'smagneticfieldanditscoronatoincreaseourunderstandingofthecausesofsolarvariabilityandtheoriginsofsolaractivity. HinodewaslaunchedsuccessfullyinSeptember2006.

Thispostergivesanoverviewofthethreeinstrumentson-boardtheHinodespacecraft: SolarOpticalTelescope(SOT),X-RayTelescope(XRT)andEUV imagingspectrometer(EIS).Severalsignificantobservationalresultsobtainedduringthefirst3.5yearsofmissionoperationsarealsopresented.

NASA SDO,itsscienceandtheUCLandata-hubRobertWalsh (UniversityofCentralLancashire)

with S. Dalla, D. Bewsher, B.J.I. Bromage,D.S. Brown, S.A. Chapman, M. Marsh, J. Pearson,

C. Alexander, and J. Kelly

LaunchedonFebruary11, 2010, theSolarDynamicsObservatory(SDO) willrevolutioniseourunderstandingoftheSunwithitsexcellenttemporalresolutionandcontinuousfulldiskcoverage. Thispresentationwillhighlightthescientificaimsofthemissionandhowitsthree-instrumentsuitewillprovideawealthofopportunitiesfornewdiscoveries. Inparticular,wewillemphasizethechallengesassociatedwiththeapproximateterabyteperdaysizeofthedatasetandwillpresenttheSDO/AIA datahubbeingsetupattheUniversityofCentralLancashire. Further, wewilloutlinehowtheUKsolarcommunitywillbeabletointeractwiththehubintheverynearfuture.

P10TheWFCAM ScienceArchive

RobBlake (RoyalObservatoryEdinburgh)withNigel Hambly, Eckhard Sutorius, Mike Read,Nick Cross, Ross Collins, Mark Holliman, and

Peredur Williams

InfraRedDeepSkySurveysoftheNorthernHemisphere

TheWFCAM ScienceArchive(WSA) isamature,databasedriven, webaccessibleproductprovidingaccesstodatatakenbytheWFCAM instrumentonUKIRT aspartoftheUKIRT InfraRedDeepSkySurveys(UKIDSS).

Thedataareavailableaspixeldata(inmulti-extensionFITS files), jpegimages(includingcolourimageswhereavailable), aswellasfullyqueryablerelationaldatabasescontainingfullinformationonalldetections.

AswellasUKIDSS data, theWSA alsocontainsneighbourtablesrelatingUKIDSS detectionstothoseofothersurveys(including2MASS,2XMM,MGC,andsixdatareleasesfromtheSloanDigitalSkySurvey). Forconvenience, alloftheseexternalcataloguesarealsoavailabledirectlythroughtheWSA interfacesothatdetectionscanbeinstantlyqueriedinallsurveys.

February2010sawtheseventhUKIDSS datarelease(DR7)containingover105millionsourcescoveringover3,000squaredegreesacrossthreeofthesurveys(theLargeAreaSurvey, GalacticClustersSurvey, andDeepExtragalacticSurvey)withdepthsofuptomagnitude22.4. A further770millionsourcescoveringover1,300squaredegreesareduetobeaddedshortlywiththeadditionoftheGalacticPlaneSurvey(GPS) intoDR7.

WepresentanoverviewofthelatestfeaturescontainedinDR7whichareavailabletoregisteredusers, aswellascoveringthefeaturesnowaccessibletoeveryoneinourlatestworldrelease(DR4).

DataIntegrationinHeliophysicsJohnBrooke (UniversityofManchester)with

Anja LeBlanc

HeliophysicsisarelativelynewdisciplinethatexplorestheSun-SolarSystemConnection.Althoughtheindividualcommunitiesinvolvedinheliophysicsarewellestablished, theyhaveevolvedindependentlyandcurrentlyitisextremelydifficulttofindandcomparedatafromacrossthediversesetofexistingdataarchives. WedescribetheuseofmethodsderivedfromtheSemanticWebtoaddressthisproblem. Wehaveintegrateddescriptionsofdatatodevelopanabstractheliophysicsdomainontology, whichcanbethoughtofasacontrolledvocabularyenrichedwithrulesthatcanbereasonedaboutbymachines. Theaimofthisontologyisbeusedtomapdata(describedbydatamodels)fromdifferentregionsoftheheliosphere. Wearealsodevelopinganontologyforcoordinatesystems,whichcandeterminewhethercoordinatesystemscanbetranslatedintoeachotherandifso,whetherthetimeisaparameteroftheoperation.Wealsodescribeworkflowswhichuseanontologytofindrelevantdatasets, e.g. whichusesanabstracttermsuchas"flare"toquerydatasetsfromtheHESSI flarelist, YOKOH flarelist, KSOflarelist. Theworkflowfindsoverlappingevent

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datafromdifferentsources, itfindstherelevanttimeintervaandlooksuptheeventlist, andcheckswhetherallinstrumentshavedatatothiseventandreturnsonlyeventsanddatawhichoverlapeachother. ThisworkispartoftheHELIOprojectfundedbytheEU intheFP7programme,seehttp://www.helio-vo.eu/

TheSuperWASP publicarchiveOliverButters (UniversityofLeicester)with

R.G. West, D. Pollacco, C. Hellier, A.C. Cameron,and WASP Consortium

TheSuperWASP (WideAngleSearchforPlanets)projectistheworld'sleadingtransitingexoplanetsurvey. Itconsistsoftworoboticobservatories(oneintheNorthernhemisphereandtheotherintheSouthernhemisphere)thatconstantlymonitorthenightsky. Imagesaretakensimultaneouslyfromeightwide-anglecamerasineachcase. Datafirststartedtobetakenin2004, sincethenthedatasethasbeenextensivelysearchedfortransitingexoplanets. Other(nonexoplanet)sciencehascomefromthedataalso, suchasthecorrelationofROSAT sourceswithvariablestarsandasteroidstudies, butthereisstillawealthofothersciencethatcanbedonewiththedata. WiththisinmindweannouncethefirstpublicdatareleaseoftheSuperWASP archive.

Thisfirstdatarelease(DR1)startsin2004intheNorthand2006intheSouthandstretchesto2008inbothcases. Thiscorrespondstojustunderfivemillionimages, each7.8x7.8degrees. Fromtheseimagesover100billiondatapointshavebeenextractedforover20millionuniqueobjects. TheSuperWASP publicarchivemakesallthisdatasearchableanddownloadableviaawebinterfacehostedattheUniversityofLeicester.

VOeventstriggeredbygravitywavesTobiaCarozzi (Univ. ofGlasgow)with

Norman Gray, and Graham Woan

VirtualObservatoryevents(VOevents)areXMLbasedmessagesthatdescribeastronomicalevents.TodatedespitethediversityofVOevents, rangingfromsupernovaeto γ−raybursts, theyhaveallbeenofelectromagneticorigin. Inthiswork, welookathowtheVOeventframeworkcanalsobeuseddescribeeventsofagravitionalorigin. WealsolookathowVOeventscanbepropagatedfromtheLIGO-VirgoAlertSystemtoVOeventsubscribersusingtheExtensibleMessagingandPresenceProtocol(XMPP).

NativeSyntheticImagingofSmoothedParticleHydrodynamicsSimulations

DuncanForgan (SUPA,IfA,UniversityofEdinburgh)with Ken Rice

I willpresentanewnumericalmethodforcreatingsyntheticobservablesfromSmoothedParticleHydrodynamics(SPH) simulations. ItemploysMonteCarloRadiativeTransfer(MCRT) techniquestoemulatethetransmissionofphotonsthroughamedium, incorporatingbothabsorptionandscattering, capturingthemonanimageplaneinamanneranalogoustothecaptureofphotonenergyonaCCD.

UnlikepreviousattemptsatimagingSPH fields, Iemployraytracingtechniquesthatdonotrequiregridding, preservingthesimulation'snativeresolvingpower. Thecodealsousesalgorithmsoriginallydevelopedforcomputergraphicsproblemstooptimiseitsefficiency.

ThismethodthereforeprovidesadirectlinkbetweenSPH simulatorsandobservers, allowingmoreconcreteobservationalpredictionstobemade. I willillustratethisbyimagingSPHsimulationsofprotostellardiscsystemstodeterminewhatfeaturescanberesolved, e.g. discspiralarmsorembryonicprotoplanets.

NewinfraredandopticalimagesservicesintheVO

NigelHambly (UniversityofEdinburgh)withM.S. Holliman, M.A. Read, and R.G. Mann

ThisposterdescribesnewSimpleImageAccess(SIA) servicespublishedtotheVirtualObservatorybytheWideFieldAtronomyUnitattheInstituteforAstronomy, UniversityofEdinburgh. Intheinfrared, weprovideimagesfromthelatestreleasesfromUKIDSS,including1000sofsquaredegreesfromthewide-angle, shallowsurveysin1.0to2.5micronpassbands(YJHK).Intheoptical,weprovideanall-skySIA cut-outservicebasedonthelegacySchmidttelescopephotographicsurveys(epoch1949-2000)asdigitisedbythenowdecommissionedprecisionplatescanningfacilitySuperCOSMOS.EverypartoftheskyiscoveredinBRI withatleasttwoepochsinR;multiple-epochimagesareavailableinthesubstantialsurveyoverlapregions. Furthermore, specialistregionshaveadditionalfilter/epochcoverage, e.g. HalphaandmatchedR exposuresintheGalacticPlane,andaround200multi-epoch/colourimagesspreadover30yearsintheESO/SRC surveyfield287at21h28m, -4500(B1950).

TheseserviceshavebeenpublishedtotheVOthroughtheWFAU publishingregistry, whichcanbefoundthroughtheIVOA RegistryofRegistries.

VirtualObservatoryServicesatWFAUMarkHolliman (UniversityofEdinburgh, Institute

forAstronomy)with Mike Read

TheWideFieldAstronomyUnithostsanumberofVirtualObservatory(VO) servicesthatenableaccesstobothdataandprocessingapplicationshousedonourserversinEdinburgh. Theseservicesprovideastronomerswithapowerfulsetoftoolsforobtainingandprocessingdatainwaysunattainablethroughconventionalaccessmethods. TheservicesofferedincludeconesearchandADQL accesstoanumberofmajordatabasesdevelopedbyourdatacentresuchasUKIDSS,SuperCOSMOS ScienceArchive, andthe6dFGalaxySurvey, andalsomanymirrorsofimportantdatabasesdevelopedelsewhere, suchasSDSS,IRAS,and2XMM .ImagesforUKIDSS andSuperCOSMOS areaccessiblethroughSIAservices. ThereareusefuldataprocessingtoolsliketheSTILTS libraryfortablemanipulation, adataminingtoolforclassificationusingkerneldensityanalysis, andaserviceforconvertingVOTablesintoKML foruseinGoogleSky. AlsohostedareanumberofVO infrastructureserviceslikeafullregistryandVOSpacethatenableuserstofindresourcesandstoredatainanonlineaccessiblelocation. WFAU providessecuredVOservicestotheproprietaryUKIDSS releases, whicharethefirstsecuredVO servicesforamajorproprietarydataresourceintheentireVO.WithalimitedknowledgeofpythonandacopyoftheVODesktopsoftwareastronomerscanscriptupworkflowsthatutilizetheseservicestoperformcomplexoperationslikecrossmatchingbetweendisparatedatasetsorextractingcataloguesfromimagesremotely. Sincemanyofourdatabasesaretoolargetobedownloadedandaccessedlocallytheseservicesmakeitpossibletoaccomplish

complicatedtasksonlineandondedicatedhardware. WFAU’slistofVO serviceswillcontinuetogrowasnewIVOA standardsareimplementedandwiththeadditionofnewdatasetsliketheVISTA surveys.

GraphicInterfacestoExplanatoryAnalysisofAstronomicalImageDatabases

AvonHuxor (UniversityofBristol)with S. Phillipps

Inthisposterwewillpresentongoingworkinwhichearlydesignsforavisualinterfacetomassiveimagingdatabases, suchasSDSS,areoutlined. Althoughmanytoolsforthepresentationandanalysisofcataloguedataareavailable(e.g.TOPCAT),theserequirethattheimagedataisprocessedintointomoreabstract, typicallyquantitative, properties. Howeverintheexploratoryphaseofthescientificprocessthepropertiespresentinthecataloguesmaynotberelevant. Moreover, thelessonsfromCSCW(computer-supportedcollaborativeworking)showthatprematureformalisation(ShipmanandMarshall1994)mayhinderproductivity. Inearlierwork(Huxor1994), weshowedthevalueofamixedinterfacecombiningtheformalnotationofknowledge-baseswiththeinformalcomponentoffree-text. Weshowhowthisinterfacedesigncanbeextendedtoprovidesupportfortheexploratoryanalysisofastronomicalimagedatabases. Thisallowstheusetomanipulatetheformal'tags'associatewiththeimagesofobjectsofinterest,supportingbothformalandinformalreasoning.

Developingskillsfor“softwareastronomy”: aninnovativedistancelearningprojectforOpen

UniversitystudentsMarkJones (TheOpenUniversity)with

James Smith, and Alan Cayless

Theabilitytoaccesslargeastronomicaldatasetsremotelyandthedevelopmentofvirtuallearningenvironmentstogetherprovideaframeworkwhichpotentiallyallowsstudentstoconductastronomicalresearch. However, theexistenceofsuchsystems, initself, isnotsufficienttofacilitatetheeffectivedevelopmentofskillswhichwouldallowundergraduatestudentstomakeappropriateuseoftheavailabledata. HerewedescribeaprojecttoallowgeographicallyseparatedstudentstoworktogethertoformacompositequasarspectrumfromdatafromtheSloanDigitalSkySurvey. Drawingontheresultsofasmall-scalepilotstudy, wedescribethedesignanddevelopmentoftheteachingmaterialtosupportthisproject. Wediscusstheparticularchallengesposedindevelopingstudentsintheinformationhandlingandinformationliteracyskillswhicharerequiredtoconduct“databaseastronomy”.

SupportingDistributedScience: RunningGalaxyZoo

ChrisLintott (UniversityofOxford)withArfon Smith, and GalaxyZooteam

Sinceitslaunchin2007, GalaxyZoohasgrowntobetheworld'slargestastronomicalcollaboration,involvingmorethan250,000membersofthepublicinclassifyinggalaxies, simulatingmergersandhuntingforsupernovae. Developingandsupportingtheinfrastructurenecessaryforsuchalargeprojectbringschallengesofscalabilitythatmostmodernastronomyprojectsface. I willreviewthesolutiontheGalaxyZooteamhavefoundforsupportingsuchprojects(involvingextensiveuseofwebservicesandhostinginthecloud)alongwiththemethodsdevelopedtoturnrawclicksintoscience. Finally, I willconsiderthe

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impacttheavailabilityoflargenumbersofvolunteerswillhaveonfuturesurveysandprogramssuchastheLSST.

SoftwaretoolsforprocessingRHESSI visibilitiesAnnaMariaMassone (CNR-SPIN) with

Michele Piana

RHESSI imagingconceptistheoneofimagemodulation: theninepairsofrotatingRHESSIgridsprovideatemporalmodulationofthearrivingflux, whosepatternrepresentsaspecificsetofspatialFouriertransformofthesource. Thesecomplexdata, thepurestformoftheRHESSI datastream, arecalledvisibilities. ThistalkwillfirstdescribeanewsoftwaretoolforthecreationofregularizedelectronvisibilitiesassociatedtothephotonvisibilitiesmeasuredbyRHESSI.Thissoftwareprovidesthesolarphysicscommunitywithaneffectiveimagingspectroscopyprocedurewhereelectronmapsoftheflaringsourcearesynthesizedatdifferentelectronenergychannelsandasmoothingconstraintalongsuchenergiesisautomaticallyimposed. Thenaninterpolation/extrapolationimagingmethodwillbepresented, forthereconstructionofmapsfrombothphotonandelectronRHESSI visibilities.

ThehierarchicalstabilityofexoplanetarysystemsofBinarystarsusingtheCaledonianSymmetric

Four-Bodymodelwithanewglobalregularisationalgorithmtohandlecloseencounters

BonnieSteves (GlasgowCaledonianUniversity)with Anoop Sivasankaran, and Winston Sweatman

TheCaledonianSymmetricFourBodyProblem(CSFBP) (StevesandRoy, 2001; Szell, StevesandErdi, 2004: andShoaib, StevesandSzell, 2008)isarestrictedfourbodygravitationalmodelrelevanttothestudyofthestabilityandevolutionofsymmetricquadruplestellarclustersandexoplanetarysystemsoftwoplanetsorbitingabinarypairofstars. OneofthemaindifficultiesinstudyingtheCSFBP wasthefailingofthenumericalintegrationalgorithmtomaintainconservationofenergyandangularmomentumnearsingularitieswhichoccurredattwo-bodycloseencounters. RecentlywehavedevelopedaregularizationalgorithmtostudycloseencountersandcollisioneventsoccurringintheCSFBP(Sivasankaran, StevesandSweatman, 2009, 2010).

Inthisposterpaper, wewillillustratethat, thedevelopedregularizedalgorithmiscapableofhandlingthetwo-bodycloseencountersefficientlybyinvestigatingasetofCSFBP orbitscontainingcloseencounterevents. Theproposedregularisationalgorithmhasbetternumericalaccuracyandenergyconservingproperties. ItisnowpossibleforustoapplytheCSFBP modeltostudythestabilityandevolutionofsymmetricexo-planetarysystemsoftwoplanetsorbitingabinarystarsystem, includingthosesystemswhichpassthroughcloseencounters. WehavenumericallyverifiedthatthehierarchicalstabilityofthesystemdependsonananalyticalstabilityparametercalledtheSzebehelyconstant. TheSzebehelyconstantisafunctionofthetotalenergyandangularmomentumofthesystemanditdependsonlyontheinitialconditionsofthesystem. UsingthenewregularisationmethodforawiderangeofSzebehely'sconstantandinitialconditions, weareabletoverifythefour-bodyanalyticalstabilitycriterionofStevesandRoy(2001)andgiveanoverallstabilitycriterionforpairsofexo-planetsorbitingsymmetricbinarystarsystems.

P11Dodarkmatterhaloshavecusps?

ChrisBrook (JeremiahHorrocksInstitute, UCLan)

PureN-bodysimulationshaveshownthatcolddarkmatterhaloshavesteepinnerdensityprofiles,or"cusps". Yetobservationsofrotationcurvesofdiskgalaxiesinferaflatter, coredinnerdensityprofile. Usingselfconsistentcosmologicalgalaxyformationsimulations, weshowthattheinclusionofbaryons, whicharedynamicallysignificantintheinnerregionsofhalos, candramaticallyaltertheprofileofthedarkmatter. Oursimulationsresultin"bulgeless"diskgalaxieswithdarkmattercores.

Extremevaluestatistics: predictingthefrequencyofthedensestclustersandsparsestvoids

OlafDavis (Oxford)with Stephane Colombi,Julien Devriendt, and Joe Silk

Oneinterestingpropertyofrandomfields- suchastheobserveddensityfieldoftheuniverse- isthedistributionoftheirhighestmaximaandlowestminima. Inparticular, themaximaofthedarkmatterfieldtranslatetothethelocationsofthemostmassiveclusters, whichexistinthehighlynon-linearregimeofgravitationalclusteringandprobetheevolutionofthepowerspectrumundergravity.

TorelatethetheoreticalmaximaoftheDM densitywithobservedmaximainasmallregionoftheuniverserequiresanunderstandingofthebehaviourofsamplemaxima: thisisthedomainofextremevalueorGumbelstatistics.

Wepresentanalyticalcalculationswhichcanpredictthedistributionofsuchmaximaandminimafromtheunderlyingpowerspectrum, anddemonstrateagoodagreementwithsimulatedGaussianfields. WealsocompareourpredictionstotheHorizon4Πsimulation, acosmologicalscaledarkmattersimulationcontaining70billionparticles.

Potentialapplicationswillbediscussed, includinglikelihoodconstraintsonvoidcosmologies, andapplicationtoobservedCMB anomaliessuchasthecoldspotand'AxisofEvil'.

Probingthedarkmatterhalosofearly-typegalaxiesvialensing

IgnacioFerreras (UniversityCollegeLondon–MSSL)

Thecombinationofgravitationallensingongalaxyscalesandstellarpopulationsynthesisenablesustoconstrainthebaryonfractioningalaxies,probingtheinterplaybetweenthedarkmatterhaloandthebaryonphysicstransforminggasintostars.I willpresentrecentworkbasedonasampleofstrong(early-type)lensesfromtheCastlessurvey.Thecombinationofanon-parametricapproachtothelensingdataandtheanalysisoftheHST/NICMOS imagesofthelensgivearemarkablygoodagreementbetweenbaryonandlensingmassintheinnerregions. Theradialtrendofthebaryonfractionoutto4-5 Re isshown,alongwithitsconnectionwiththeFundamentalPlane. I willputthisresultincontextwithrecentestimatesoftheglobalbaryonfractioningalaxies.

Cosmologyonsmallscales: thestructureof(mostly)darkmatterhalos

CarlosFrenk (DurhamUniversity)

Thestandardmodelofcosmology- the"Λcolddarkmatter"model- isbasedontheideathatthedarkmatterisacollisionlesselementaryparticle,probablyasupersymmetricparticle. Thismodelhasbeenfamouslyverifiedbyobservationsofthecosmicmicrowavebackgroundradiationandthelarge-scaledistributionofgalaxies. However, themodelhasyettobetestedconclusivelyonthesmallscalesappropriatetomostastronomicalobjects, suchasgalaxiesandclusters. I willreviewourcurrentunderstandingofthedistributionofdarkmatteronsmallscaleswhichderiveslargelyfromlargecosmologicalN-bodysimulationsandIwilldiscussprospectsfordetectingdarkmatter,eitherthroughitsgravitationaleffectongalaxiesandclustersor, moredirectly, through γ−rayannihilationradiation.

SuddenFutureSingularitymodelsasanalternativetoDarkEnergy?

HodaGhodsi (UniversityofGlasgow)withMartinA. Hendry

Oneofthekeychallengesfacingcosmologiststodayisthenatureofthemysteriousdarkenergyintroducedinthestandardmodelofcosmologytoaccountforthecurrentacceleratingexpansionoftheuniverse. Inthisregard, manyothernon-standardcosmologieshavebeenproposedwhichwouldeliminatetheneedtoexplicitlyincludeanyformofdarkenergy. OnesuchmodelistheSuddenFutureSingularity(SFS) model, inwhichnoequationofstatelinkingtheenergydensityandthepressureintheuniverseisassumedtohold. Inthismodelitispossibletohaveablowupofthepressureoccurringinthenearfuturewhiletheenergydensitywouldremainunaffected. TheparticularevolutionofthescalefactoroftheUniverseinthismodelthatresultsinasingularbehaviourofthepressurealsoadmitsaccelerationinthecurrenteraasrequired. InthiscontributionIwillpresenttheresultsofthetestsofanexampleSFS modelagainstthecurrentdatafromhighredshiftsupernovae, baryonacousticoscillations(BAO) andthecosmicmicrowavebackground(CMBR).WeexplorethelimitsplacedontheSFSmodelparametersbythecurrentdatathroughemployinggrid-basedandMCMC searchmethods. ThisletsusdiscusstheviabilityoftheSFS modelinquestionasanalternativetothestandardconcordancecosmology.

LoCuSS:WeakLensingAnalysisof21GalaxyClustersatz=0.15-0.3

VictoriaHamilton-Morris (UniversityofBirmingham)with G.P. Smith, E. Egami, T. Targett,

C. Haines, and A. Sanderson

TheLocalClusterSubstructureSurvey(LoCuSS) isamulti-wavelengthsurveyof100X-rayluminousgalaxyclustersat0.15< z < 0.3, spanningX-raytoradiowavelengths. OneofthemainsciencegoalsistomeasurethesubstructureoftheDarkMatterdistributionwithinclustersandtocorrelateclustersubstructurewithresidualsonclustermass-observablescalingrelations. I willpresentadetailedstructuralanalysisof21clustersusingourHST/ACS SNAPSHOT data. Substructuresfoundinthe"non-parametric"lensingmassmapsarecomparedwithK-bandluminositymaps, andChandraX-rayfluxmaps. Thesethreeindependentprobesareincloseagreement, includingbothstructuresdetectedwithintheACS fieldsofview,and(inasub-setofclusters)structureslocated

56 P10–P11

outsidetheobservedACS fields. Usingthenear-IRdataasaprioronboththelocationandmassofsubstructureswithintheclusters, wethenuseaBayesianmethodbasedonLenstool(Julloetal.,2007), tofitmultipledarkmatterhaloestothesheardata. Ourobservationalresultsonthecomplexityoftheclustermassdistributionsarecomparedwiththeoreticalpredictionsofclustersubstructure.

TheZEPLIN-III DarkMatterSearchExperimentMarkusHorn (ImperialCollegeLondon)

TheZEPLIN-III experimentattheBoulbyUndergroundLaboratoryusesa12-kgtwo-phaseXenontimeprojectionchamberspecificallydesignedtosearchforDarkMatterWIMPs. Thedetectormeasuresbothscintillationandionisationsignalstodiscriminatebetweendifferentparticlespeciesinteractinginthedetector. ThisallowsnuclearrecoilsignaturesofWIMPstobeseparatedfromthemorenumerousbackgroundofeventsgeneratedbyphotonsandelectrons. Theresultsfromthefirstsciencerun, withapprox850kgdaysdataacquiredin2008, arepresented. Additionallythecurrentupgradeoftheexperimentwithnewultra-low-backgroundphotomultipliersandtheinstallationofaneutronvetoisshown. Theprospectiveoutcomeoftheforthcomingsecondsciencerunisthendiscussed.

A NewPixonWeakLensingClusterMassReconstructionMethod

DanielJohn (DurhamUniversity)with V.R. Eke,and L.F.A. Teodoro

Wepresentanewpixon-basedmethodforclustermassreconstructionsusingweakgravitationallensing. Pixonsareanadaptivesmoothingschemeforimagereconstruction, wherethelocalsmoothingscaleisdeterminedbythedata. Wealsointroduceanewgoodness-of-fitstatisticbasedontheautocorrelationoftheresidualsoftheshearfield. WetestouralgorithmonsimulatedlensingdatasetsusingNFW haloswithandwithoutsubstructure. WecompareourresultstopreviousmethodssuchasKaiser-Squires(KS), MaximumEntropy(ME) andtheIntrinsicCorrelationFunction(ICF ) andshowanincreasedaccuracyinthemassreconstructions. Wefinallydiscussfutureapplicationstodata.

WeighinggalaxiesusinggravitationallylensedSNLS supernovae

JakobJonsson (UniversityofOxford)withM. Sullivan, I. Hook, S. Basa, R. Carlberg,

A. Conley, D. Fouchez, D.A. Howell, K. Perrett,and C. Pritchet

Gravitationallensingbyforegroundmattercanmagnifyorde-magnifybackgroundsources.Standardcandles, liketypeIasupernovae(SNeIa),canthereforebeusedtoweightheforegroundgalaxiesviagravitationallensing. Wepresentconstraintsondarkmatterhalopropertiesobtainedusing175SNeIafromthefirst3-yearsoftheSupernovaLegacySurvey(SNLS).Thedarkmatterhaloofeachgalaxyintheforegroundismodelledasatruncatedsingularisothermalspherewithvelocitydispersionandtruncationradiusobeyingluminositydependentscalinglaws. Wecannotconstrainthetruncationradius, butthebest-fittingvelocitydispersionscalinglawagreeswellwithresultsfromgalaxy-galaxylensingmeasurements.ThenormalisationofthevelocitydispersionscalinglawsarefurthermoreconsistentwithempircalFaber-JacksonandTully-Fisherrelations.Wehavealsomeasuredthebrightnessscatterof

SNeIaduetogravitationallensing. ThisscattercontributesonlylittletotheSNLS sample(z < 1),butwouldcontributesignificantlyat z > 1.6.

Theimpactofdelensinggravitationalwavestandardsirensondeterminingcosmological

parametersCraigLawrie (UniversityofGlasgow)with

Martin Hendry, Fiona Speirits, and Joshua Logue

Recentlytherehasbeenmuchattentioninthecosmologyliteratureonthepotentialfutureuseofcompactbinaryinspirals, so-calledgravitationalwavestandardsirens, ashighprecisionprobesoftheluminositydistanceredshiftrelation.

Ithasbeenrecognised, however, thatweaklensingduetointerveninglargescalestructurewillsignificantlydegradetheprecisionofstandardsirens. Shapiroetal(2010)presentamethodfor"de-lensing"sirens, bycombininggravitationalwaveobservationswithmapsofcosmicshearandflexionalongeachsiren'slineofsight.

Inthispresentationweexploretheimpactofthisde-lensingprocedureforconstrainingcosmologicalparameters. UsingMonteCarlosimulationsweinvestigatetheaccuracywithwhichthedimensionlessdensityparametersmaybedetermined, beforeandafterde-lensing, withfuturedatafromtheproposedLISA satelliteandEinsteinTelescope.

DirectdetectionofdarkmatterPawelMajewski (RutherfordAppletonLaboratory)

DarkMatterisoneofthegreatestmysteriesinscience. Althoughitmakesuproughly25%oftheuniverse, ithasneverbeendirectlydetected. Forlastdecadesthehuntfordetectionofdarkmaterparticlehasacceleratedandbecameamotivationtomanyofingeniousexperimentsaroundtheworld. I willpresentreviewofexistingandplanneddarkmatterdirectdetectionexperimentswithfocusonthevarietyofimplementedexperimentaltechniques.

Theimpactofdarkmattercuspsandcoresonthesatellitegalaxypopulatio

JorgePenarrubia (UniversityofCambridge, IoA)with A. Benson, M. Walker, G. Gilmore,

A. McConnachie, and L. Mayer

InthistalkI willshowtheresultsfromN-bodysimulationsthatstudytheeffectsthatadivergent(i.e. "cuspy")darkmatter(DM) profileintroducesonthetidalevolutionofdwarfspheroidalgalaxies(dSphs). I willshowthattheresilienceofdSphstotidalstrippingisextremelysensitivetotheslopeoftheinnerhaloprofile. I willalsooutlinetheresultsfromcalculationsthatsimulatethehierarchicalbuild-upofspiralgalaxiesassumingdifferenthaloprofilesanddiscmasses, whichshowthatthesize-massrelationestablishedfromMilkyWay(MW)dwarfsstronglysupportsthepresenceofcuspsinthemajorityofthesesystems, ascoredmodelssystematicallyunderestimatethemassesoftheknownUltra-FaintdSphs. ThesemodelsalsoindicatethatamassiveM31discmayexplainwhymanyofitsdSphsfallbelowthesize-massrelationshipderivedfromMW dSphs. WealsouseourmodelstoconstrainthemassthresholdbelowwhichstarformationissuppressedinDM haloes,findingthatluminoussatellitesmustbeaccretedwithmassesabove 108--109Msol inordertoexplainthesize-massrelationobservedinMWdwarfs.

DarkMatterintheMilkyWayJustinRead (UniversityofLeicester)

Experimentsdesignedtodetectadarkmatterparticleinthelaboratoryneedtoknowtheverylocalphasespacedensityofdarkmatter, bothtomotivatedetectordesignandtointerpretanyfuturesignal. I discussrecentprogressonestimatingthisanditsimplications.

UnmodifiedGravityFergusSimpson (Edinburgh)with Brendan Jackson,

and John Peacock

Byrelaxingtheconventionalassumptionofapurelygravitationalinteractionbetweendarkmatteranddarkenergy, substantialalterationstothegrowthofcosmologicalstructurecanoccur.AsanillustrationI willexplorethecaseofexcessdarkmatterformingfromadecayingdarkenergycomponent. Simpleanalyticsolutionstothemodifiedgrowthratesarefoundforthesemodels.Furthermore, neglectingthesedarksectorinteractionscaninduceasignificantbiasintheinferredgrowthrate, potentiallyofferingafalsesignatureofmodifiedgravity.

Wave-mechanicsofLargeScaleStructureEdwardThomson (UniversityofGlasgow)with

MartinA. Hendry, and LuisF.A. Teodoro

SimulationsofLargeScaleStructureusingN-Bodycodeshavehelpeddefinethe Λ−CDM paradigm.WhileN-Bodycodesremainthemostpopularapproach, alesserknownmethodwasdevelopedintheearly90'sthatformulatestheequationsdescribinglargescalestructure(LSS) formationwithinawave-mechanicalframework. ThismethodcouplestheSchroedingerequationwiththePoissonequationofgravity. Thewavefunctionencapsulatesinformationaboutthedensityandvelocityfieldsasasinglecontinuousfieldwithcomplexvalues.

InthispresentationI willreviewsomeofthekeyfeaturesofthewave-mechanicalapproachtoLSS.Themethodavoidstheadditionofanartificialsmoothingparameter, asseeninN-bodycodes,andisabletofollow'hotstreams'- somethingthatisdifficulttodowithphasespacemethods. ThemethodiscompetitivewithN-bodycodesintermsofprocessingtime. Thewave-mechanicalapproachcanbeinterpretedintwoways: (1)asapurelyclassicalsystemthatincludesmorephysicsthanjustgravity, or(2)astherepresentationofadarkmatterfield, perhapsanAxionfield, wherethedeBrogliewavelengthoftheparticlesislarge.

EmpiricalConstraintsontheDarkMatterContentofDwarfSpheroidalGalaxies

MatthewWalker (InstituteofAstronomy,UniversityofCambridge)

Thedwarfspheroidal(dSph)galaxiesorbitingintheMilkyWay'shaloarethesmallest, faintestanddarkestknownobjectsforwhichinternalkinematicsimplyadarkmattercomponent. HereIdiscussconstraintsonthedensityprofilesofdSphdarkmatterhalosasderivedfromobservedstellarkinematics, andI assessthevalidityandeffectsofvariousmodelingassumptions. I considerrealisticobservationaluncertaintiesinthecontextofeffortstodetectdarkmatterindirectlyintheformofhigh-energyphotonsreleasedduringself-annihilationevents. I attempttoidentifythemostsuitabledSphtargetsforsuchsearches.

P11 57

P12TheFrequencyandCompositionofWater-Rich

ExtrasolarAsteroidsJayFarihi (UniversityofLeicester)with

M.A. Barstow, S. Redfield, P. Dufour, andN.C. Hambly

Theinterstellarmediumisnolongeraviablephysicalmodelfortheoriginofheavyelementsseenincoolwhitedwarfs. Instead, ongoingSpitzerandground-basedstudiesofalargenumberofsingle, metal-enrichedstarshavedemonstratedthesourceofthepollutionmustbecircumstellar. Wheredetected, thegeometryofthedustand(heavyelement)gasdisksorbitingcontaminatedwhitedwarfsareconsistentwithtidallydisruptedasteroidanalogs, ahypothesiswhichalsoaccountsforthevolatile-poor, rockycompositionofthephotosphericmetalsandcircumstellardebris. Tantalizingly, ahandfulofthesepollutedwhitedwarfsappeartocontainexcesshydrogen, anindicationthatthedestroyedminor(ormajor)planetcarriedinternalwater.

I willdescribetheevidenceforsuchwater-richextrasolarasteroids, andtheongoingworktoconfirmthishypothesisbysearchingforoxygeninexcessofthatexpectedfrommineraloxidesascommonlyfoundintheinnerSolarSystem. Theconfirmationofwaterinextrasolar, terrestrialplanetarybodieswillconstrainthefrequencyofenvironmentsfavorabletohabitableplanetformationandmayindicatethathabitatssuitabletoextremophilesarecommonintheGalaxy.

TheMain-BeltComets: Long-livedIceintheInnerSolarSystem

HenryHsieh (QueensUniversityBelfast)

Themain-beltcometsareanewly-identifiedclassofsmallbodiesinoursolarsystemwhichhavetheorbitsofmain-beltasteroidsbutexhibitcometaryactivityintheformofdusttailsorcomae,indicatingthepresenceofsublimatingice. Sincetheirdiscoveryin2006, theyhavedrawninterestduetotheunexpectedpresenceoficybodiesonstable(i.e. long-lived)innersolarsystemorbits,theirimplicationsforsolarsystemformation, andtheirastrobiologicalsignificanceasapossibleprimordialterrestrialwatersource. I willdetailtheadvancesmadeinthestudyoftheseunusualobjectssincetheirdiscovery, discussthemanyoutstandingquestionsthatstillremain, andconsidertheirroleinourunderstandingoftheoriginandpastandpresentdistributionofwaterinthesolarsystem.

NightsidePollutionofExoplanetTransitDepthsDavidKipping (Harvard-SmithsonianCenterfor

Astrophysics)with G. Tinetti

Hot-Jupiterexoplanetshavebeendiscoveredtoexhibitsignificantthermalemissionfromtheirdaysidebutefficientcirculationimpliessimilaremissionsignalsfromthenightsidetoo. Thisemissionactsasaself-blendandattenuatestransitdepths, particularlyatmid-infraredwavelengths.TheeffectisshowntocausechangesintheSpitzer-measuredtransitdepthsatthe1-σlevelforthecaseofHD 189733b. Weexplorehowthenightsidepollutioneffectalterstheinterpretationofexoplanetspectra, withemphasisonthesignatureofwater, andalsopresentmethodsforaccountingforthisattenuation.

TheDensitiesofKuiperBeltObjectsPedroLacerda (Queen'sUniversityBelfast)

ThecoldKuiperbeltobjects(KBOs)arebelievedtocontainasignificantfractionofvolatilesintheformofice. Thefewdensityestimatesthathavebeensecuredsupportthisidea. KBO bulkdensitiescanbeconstrainedinbinaries, ifthesize(albedo)known, orfromlightcurvedata(spinperiodandphotometricrange)undertheassumptionthattheobjectsarenearhydrostaticequilibrium. OneofthemajorsciencegoalsoftheHerschelkeyprogrammetostudyKBOswillbetomeasurethealbedosofroughly25binaryKBOsandestimatethesystemdensities. Tothisdate,mostoftheusefuldensityestimateshavecomefromlightcurveanalysis. I willoutlinewhatiscurrentlyknownaboutKBO densities, includingestimatesobtainedusingthemostrecentlightcurvedata. I willdiscusspossibletrendsbetweendensityandotherphysicalpropertiesandwhatthosemightbetellingusaboutthewatercontentandinteriorstructureofKBOs.

ObservationsandmodellingofwatervapourlinesintheHerschelSPIRE FTS spectrumoftheluminousred-supergiant, VY CanisMajoris

MikakoMatsuura (UniversityCollegeLondon)with JeremyA. Yates(UCL), MichaelJ. Barlow(UCL), Dugan Witherick(UCL), Roger Wesson

(UCL), E.T. Polehampton(RAL), BruceM. Swinyard(RAL),and HerschelMESS Keyprojectconsortium

Watervapouriscommonlyfoundintheatmospheresofoxygen-richredgiantsandsupergiants. TheHerschelSpaceObservatoryhascarriedoutaspectralsurveyofluminousM-supergiantVY CanisMajorisinthefar-infraredandsubmillimetre. Inparticular, the200-670micronregionhasbeenexploredforthefirsttimeusingtheSPIRE (SpectralandPhotometricImagingReceiver)FourierTransferSpectrometer(FTS).WepresenttheSPIRE FTS observations, togetherwithnon-localthermodynamicequilibriumSMMOLmodellingofthefar-infraredwater-vapourlines,dominantcoolantsintheoutflowsfromsuchstars.

AmasingWaterAnitaRichards (JBCA,UniversityofManchester)

Thewatermoleculeisoneofthefewknowntoproducenatural, cosmicmasers. Thesecanattainextaordinarybrightnesstemperatures(1017K)whichallowstheirpositionsandvelocitiestobemeasuredwithspatialandspectralresolutionsofmilli-arcsecandtensofm/s, usingradiointerferometerssuchase-MERLIN.Masersfromwater(anditsdaughter, thehydroxylradical)arefoundinenvironmentsfromcometstodiscsorbitingAGN.I willconcentrateontheuseofwatermaserstomeasurethekinematicsofmoleculargasandshocksinstar-formingregions.Lookingahead, ALMA willimagebothmaserandthermalwater(sub-)mmlines, potentiallyexcitingindicatorsofdifferentiationinproto-planetarydiscs.

CharacterisationofexoplanetaryatmospheresIngoWaldmann (UCL)

Amongthe400-plusexoplanetsdiscoveredtodate, anever-growingsampleofthetransitingvarietypresentthemselvesasgoodtargetsforfurthercharacterisation. Usingtransmission(whentheplaneteclipsesitshoststar)andemission(theday-sidethermalemissionoftheexoplanet)spectroscopyitispossibletostudytheatmospheric

compositionsoftheseso-called"hotJupiters"inmoreandmoredetail. ThefeasibilityofsuchmeasurementshasbeendemonstratedwithgreatsuccessusingSpitzerandHST intherecentyears.Mostnotablearethedetectionsofmolecularspeciessuchaswater, methane, carbonmonoxideanddioxideinthenearinfra-redforavarietyofplanets. Thesedetectionsallowustobuildupanintricatepictureoftheatmosphericcompositionsanddynamicspresent. AttheendoftheSpitzercold-phase, agapinspace-basedobservatoriesinthenear- tomid-infra-redhasemerged, callingforincreasedeffortsinground-basedtechniques.Withthedetectionofmethaneinfluorescence, intheL-band, onHD 189733b, ithasbeenshownthatsuchmeasurementsusingmedium-sizedtelescopesonthegroundarefeasible. Atthisconference, I willgiveanoverviewofwhathasbeendonefromthespaceandground, whatwehavelearnedfromtheseobservations, andhowtobuilduponourresultsinfuturedevelopments.

P13TheInfluenceofHotPlasmaPressureon

MagnetosphericStructureatSaturnNicholasAchilleos (UCL) with C.S. Arridge, and

P. Guio

AlthoughthegiantplanetsSaturnandJupiterbothhaverapidlyrotatingmagnetospheres, andplanetarydipolemomentsfarstrongerthantheEarth's, theydifferinseveralimportantaspects. Inthispresentation, weshowresultsofforcebalancecalculationsusingtheoreticalmagnetosphericmodelsforbothplanetswhichrevealthat: (1)TheplasmadiscinJupiter'soutermagnetospherehasastructureprimarilyduetoabalancebetweenhotplasmapressureandmagneticcurvatureforce;while(2)theanalogousregionatSaturnismaintained, inaddition, byamuchstrongerrelativecontributionfromcentrifugalforceassociatedwiththerotatingplasma. TherelativesizesofthiscentrifugalforceandthevariablehotplasmapressureatSaturnalsostronglyaffectthe'compressibility'ofthekronianmagnetosphere.

AlfvénWavesinPartially-IonisedandRecombiningPlasmas

EuanBennet (UniversityofGlasgow)withDeclanA. Diver, and LuisF.A. Teodoro

TheearliestexampleofapartiallyionisedcollisionalplasmawastheUniverseduringtheepochofrecombination, about380,000yearsaftertheBigBang. Thisisthefirsttimethatneutralspecies(atoms)weremade. Inthispaper, wemodelthepropagationofAlfvénwavesthroughthecosmicplasmaasitmakesthetransitionfromfullyionizedtoalmostneutral, aspartofawiderstudyoftheplasmaphysicsoftheepochofrecombination. Infact, thisworkshowsthatitisunlikelythatAlfvénwavescouldpropagatenormally, andsoarelimitedintheinformationtheycanconveyfromtheearlymagnetisedUniverse.

WepresenttheoreticalresultsandnumericalsimulationswhichshowthattransverseMHDAlfvénwavespropagatinginaplasmathatisundergoingsignificantrecombinationwillneithersurviveintheiroriginalform, norretaincharacteristicsrelatedtotheirinitialconditions.WefindthattheAlfvénwavesaresignificantlyaffectedbytherisingneutralgaspressure, coupled

58 P12–P13

withthefallingplasmapressure, whentheplasmaismomentum-coupledtotheneutralgas.

TheplasmavelocityfielddisturbanceoftheAlfvénwaveinducessoundwavesinthegaswhich(i)carryenergyaway, depletingtheAlfvénwaveenergy, and(ii)interactfurtherwiththeplasmatoinducemagneto-sonicwaves. Inthisway, thepropagationofAlfvénwavesisconsiderablychangedbytheevolvingionizationfraction. Theimplicationofthischangeinwavepropagationpropertiesliesmainlyinthemagneticdiagnostics:weshowthatthedetectedpolarizationofmagneticfieldarisingfromAlfvénwavespropagatingthroughrecombiningmatterissignificantlyperturbedcomparedtothenon-interactingcase.

TheShockingSizeofCometMcNaughtGeraintJones (UniversityCollegeLondon–MSSL)

with GeraintH. Jones, RobertJ. Forsyth, andAndre Balogh

InJanuary/Febuary2007, CometC/2006P1(McNaught)becamethebrightestcometfor40years. TheESA/NASA Ulyssesspacecraft, inanear-polarorbitabouttheSun, performedaserendipitouscrossingofMcNaught’siontail, withitsdeepestpenetrationofthetailoccurringonFebruary7(Neugebaueretal., ApJ 667, 1262,2007), atadistanceof ∼ 1.6 AU downstreamofthecomet’snucleus. Theadditionofionizedmaterialtothesolarwindthatoccursatproductivecometsleadstotheformationofabowwave/shock, asthesolarwindflowadjuststothepresenceofthecometaryobstacle. Here, wepresentourresultsofasearchforCometMcNaught’sbowshock, primarilyusingdatafromUlysses’smagnetometerinstrument, andcomparethemtothosederivedfromobservationsmadeduringtheUlyssestailcrossingofC/1996B2(Hyakutake)in1996, andthetargetedencountersofotherspacecraftwithcomets. Theresultsrevealthevastscalesoverwhichproductivecometscanaffecttheirsurroundings.

SearchingforEvidenceofStarSpotsinSTEREOHeliosphericImagerData

RobertKidd (LancasterUniversity)with J.A. Wild,C.J. Davis, and J.A. Davies

TheHeliosphericImager(HI) experimentsonboardNASA’sSTEREO satellitesaredesignedtoobservetheinterplanetaryspacebetweentheEarthandtheSuninordertoimagetransientsinthesolarwindsuchascoronalmassejections.However, alargenumberofstarsliewithinthebackgroundofeachimage, takingseveralweekstocrosstheimager’sfield-of-view. Assuch, HIdatacanpotentiallybeexploitedtostudychangesinthelightfromthesebackgroundstars. Starspots, likeSunspots, areareasofthestellarphotospherethatarecoolerthanthesurroundingregionsandthereforevisiblydarker. Asaspotmovesacrossthediskofastar, thereisacorrespondingdropintheobservedlightintensity;weseeksuchvariationsinSTEREO HI data. Inadditiontoobservationalfindings, basedupon3yearsofHI data, firstresultsfromasimplemodeltopredictlightcurvesforvariousstarspotdistributionswillbepresented. ThismodelwilldeterminethefeasibilityofdetectingstarspotsinHI dataandplaceconstraintsonsizesofspotsthatmightbedetectedinthisway. Ultimately, thestudyofspotsonstarssimilartoourSunwillindicatelevelsofstellaractivity, andbyextensiontheseverityofso-calledspaceweather, insolar

systemsoutsideourownandplacetheextremesoftheSun’svaryingactivityinawidercontext.

TheroleofH3+inplanetaryatmospheresSteveMiller (UCL) with Tom Stallard

Thesimplemolecularion, H3+, playsacrucialroleintracingenergyinputsintotheupperatmospheresofgiantplanets: itisthusatracerofmagnetospheric-ionosphericcoupling. Butitdoesmuchmorethanthat:

1)Itactsasasourceofionisation, playingapivotalroleinthegenerationofJouleheating; 2)Itgeneratesbothion- andthroughion-neutraldrag-neutralwinds, addingtotheenergybalanceoftheupperatmosphere; 3)Itactsasastabilisingcoolant- importantinthesolarsystemandbeyond.

Waytogoforsuchalittlemolecule!

Simplemodelsforclosedfieldlineregionsofthree-dimensionalrigidlyrotating

magnetospheresThomasNeukirch (UniversityofSt. Andrews)with

Nasser Al-Salti

Wepresentamethodtocalculatesimplethree-dimensionalsolutionsofthemagnetohydrostaticequationsintheco-rotatingframeofreferenceoutsidemagnetizedrigidlyrotatingcentralbodies,e.g. planetsorstars. Wemakenosymmetryassumptionforthemagneticfield, butneglectoutflowsandspecifyaparticularformforthecurrentdensity. Themagnetohydrostaticequationscanthenbereducedtoasinglelinearpartialdifferentialequationforapseudo-potential U ,fromwhichthemagneticfieldcanbecalculatedbydifferentiation. Theequationfor U canbesolvedbystandardmethods, insomecasesevenanalytically. Thesolutionscanalsobeusedtodeterminetheplasmapressure, densityandtemperatureasfunctionsofallthreespatialcoordinates. Despitetheobviouslimitationsofthisapproach, itcould, forexample, beusedasasimpletooltocreatethree-dimensionalmodelsfortheclosedfieldlineregionsofrotatingmagnetospheresofplanetsorstarswithoutassumingrotationalsymmetry.

LaboratoryExperimentstoinvestigatethemechanismsofAuroralKilometricRadiationKevinRonald (UniversityofStrathclyde)withD.C. Speirs, S.L. McConville, K.M. Gillespie,

A.D.R. Phelps, R. Bingham, A.W. Cross,C.G. Whyte, C.W. Robertson, W. He, R.A. Cairns,

I. Vorgul, and B.J. Kellett

ElectronsdescendingthroughtheauroralregionsoftheEarth’smagnetospherearesubjecttoanincreasingmagneticfield. Conservationofthemagneticmomentassociatedwiththeelectrontrajectoriesresultsintheelectronstreamformingahorseshoedistributioninvelocityspace. Intheregionsofdepletedplasmadensity(plasmafrequency << cyclotronfrequency)powerfulradiationemissionsareobservedintheX-modeclosetothecyclotronfrequency, ∼ 300kHz. Ithasbeenspeculatedthatthisradiationisassociatedwithrelaxationofthefreeenergyintheelectrondistributionbyakineticcyclotroninstability. Itisthoughtthatsimilarprocessesoccurinmanymagnetisedastrophysicalobjects.

Toprovidefurtherinsightintothisproblem, anexperiment(scaledtomicrowavefrequenciesbyincreasingthemagneticfield)hasbeendevisedattheUniversityofStrathclydewhereanelectronstreamisinjectedintoanincreasingmagneticfield

toformcomparableelectronvelocitydistributions.Theexperimentsareconductedinparallelwithanextensivenumericalsimulationprogramme, whichaidsinthedesignoftheapparatusandintheunderstandingoftheelectrodynamics. Theseexperimentsandsimulationshaveshownstrongagreementwithconversionefficiency(fromelectronkinetictowavefieldenergy)of∼ 1 − 3%, withtheemittedradiationneartotherelativisticcyclotronfrequency, propagatingandpolarisedperpendiculartothebiasmagneticfield.Theseresultsareconsistentwiththegeophysicalobservations.

Themostrecentmeasurementshaveintroducedabackgroundplasmaintothegenerationregion, tosimulatethedepletedbackgroundplasmaintheauroraldensitycavities. Onemayanticipatethatthisplasmawillbeclosetoupperhybridabsorptionresonancefortheradiationgeneratedbytheenergeticbeam. Thisplasmahasbeennotedtosignificantlyinhibittheradiationgenerationwhenthedensityexceedsacertaincriticallevel.

RadioobservationsofhighlyenergeticpulsarsPatrickWeltevrede (JodrellBankCentrefor

Astrophysics)

InthistalkI willcomparethecharacteristicsofradiopulsarswithhighandlowspin-downenergy-lossrates. Animportantconclusionisthatofthefractionallinearpolarizationintheradiobandisveryhighforhighlyenergeticpulsars. Thetransitionappearstohappenatthedeathlinepredictedforhigh-energycurvatureradiation,suggestingapossiblelinkbetweentheemissionphysicsofthe γ−raysandtheradio.

Itisarguedthatthemostdirectlinkbetweenthehigh-energyandradioemissioncanbefoundforthesubgroupofpulsarswhichwecalltheenergeticwidebeampulsars. Thesimilaritiesinpulsemorphologysuggestthatbothtypesofemissionareproducedatthesameextendedheightrangeinthemagnetosphereandpropagationeffectsinthemagnetospherecouldplayanimportantrole. Thelatterwouldnaturallyleadtodecouplingofthewavemodes, whichcouldexplaintheobservedhighdegreeoflinearpolarization.

Thereisgrowingevidencethatthebrakingtorqueofpulsarscausestheanglebetweenthemagneticaxisandtherotationaxistoevolveovertime. Thishasimportantconsequencesforevolutionarymodelsandforestimationsofthetotalnumberofneutronstars. Theunderlyingphysicsofthechangeinmagneticinclinationisfarfromunderstoodandthevalidityofthestandardformulatoderivequantitieslikethespin-downenergylossrateappeartobequestionable.

IonlosstotheSolarWindfromVenusatSolarMinimum

AlanWood (AberystwythUniversity)withS.E. Pryse, M. Grande, and ASPERA team

TheabsenceofanintrinsicmagneticfieldonVenusallowsthesolarwindtointeractdirectlywiththeionosphereandupperatmosphereoftheplanet. ThelossofionsfromtheVenusianenvironmenttothesolarwindhasdirectimplicationsfortheevolutionoftheplanetaryatmosphere. Escapemechanismsinducedbythesolarwindarethoughttobethedominantlossprocessesatsolarmaximumforheavyatmosphericgasessuchasoxygen.

P13 59

ObservationsconductedbyVenusExpressaroundsolarminimumwereusedtobuildmapsofionsofionosphericoriginwithintheVenusianenvironment. Theseobservationsshowedasymmetriesinboththedawn-duskandnoon-midnightplanes. Inthedawn-duskdirectiongreaternumbersofionswereobservedonthedusksidethanonthedawnside. Inthenoon-midnightplanegreaternumbersofionswereobservedonthedayside, althoughsignificantnumbersofionswereseennightwardoftheterminator. Collectivelytheseobservationssuggestedanightwardionflowdrivenbytheday-to-nightpressuregradient. Theionenergiessuggestedavelocityofseveralkm/s.

Theionmapsshowedthepresenceofoxygenionsuptoaltitudesoffewhundredsofkmonthedaysideandtoseveralplanetaryradiionthenightside. Inallsectorssomeobservationsshowedionswithenergiesgreaterthanthatrequiredtoescapefromtheplanet, withthelargestenergiesobservedintheshockedsolarwind. InviewoftheseobservationstwotypesofionlossmechanismsweresuggestedtooccuratVenusatsolarminimum. Atthehighestaltitudesplasmawaslostbydirectinteractionwiththesolarwind.Atloweraltitudesthenightwardflowacceleratedionsintothetailregionandsomeoftheseionshadsufficientenergytoreachtheescapevelocity.

P14TRACE/EUV observationofdrivenloop

oscillationsIstvanBallai (UniversityofSheffield)with

David Jess

InthisstudyweuseTRACE observationstocorroborateprevioustheoreticalwork, whichdeterminedtheresponseofacoronallooptoaharmonicdriverinthecontextofidealMHD,aswellasdeterminationofthemagneticfieldandthedegreeoflongitudinalinhomogeneity.WaveletandFouriertimeseriesanalysisareappliedtoTRACE imagesoftheperiodofinterest,andthephysicalparametersofthecoronallooparedeterminedusingseismologicaltechniques.Thestudiedcoronalloopisfoundtohavetwoperiodswhichcouldbeinterpretedasbelongingtothefundamentalandfirstharmonicbutalsocouldreflectthestageofanoverdrivenloop.Usingcoronalseismologicaltechniqueswedeterminethemagneticfieldinsidetheoscillatingcoronalloop. Theobtainedvaluesarefoundtobedependentonthescenarioemployedtoexplaintheperiodsofoscillations.

LongperiodoscillationsinsunspotsNickyChorley (UniversityofWarwick)withB. Hnat, V.M. Nakariakov, A.R. Inglis, and

I.A. Bakunina

Longperiodoscillationsofthegyroresonantemissionfromsunspotatmospheresarestudied.TimeseriesdatageneratedfromthesequencesofimagesobtainedbytheNobeyamaRadioheliographoperatingatafrequencyof17GHzforthreesunspotshavebeenanalysedandarefoundtocontainsignificantperiodsintherangeofseveraltensofminutes. Waveletanalysisshowsthattheseperiodsarepersistentthroughouttheobservationperiods. Thepresenceoftheoscillationsisconfirmedbyseveralmethods(periodogram, wavelets, Fisherrandomisationandempiricalmodedecomposition). Spatialanalysis

usingthetechniquesofperiod, power, correlationandtimelagmappingrevealsregionsofenhancedoscillatorypowerintheumbralregions. Alsoseenaretworegionsofcoherentoscillationofabout25pixelsinsize, thatoscillateinanti-phasewitheachother. Possibleinterpretationoftheobservedperiodicitiesisdiscussed, intermsoftheshallowsunspotmodelandtheleakageofthesolarg-modes. Wealsopresenttheanalysisoffollowingonesunspotoverthecourseof9days, showingthestabilityofthelongperiodoscillations, inboththebrightnesstemperatureandpolarisationdata.

BigBrightPoint, SmallBrightPoint, Cardboardbox

PhilipCrockett (Queen'sUniverstyBelfast)withMihalis Mathioudakis, David Jess, Sergiy Shelyag,

and Francis Keenan

PhotosphericMagneticBrightPoints(MBPs), arethesmallestmagneticfeaturesthatarecurrentlyresolvedonthesolarsurface. Beingomnipresent,highlymagneticobjects, MBPsmayprovidedetailsonthecreation, emergenceandevolutionofthesmall-scalekilogaussmagneticfield. High-resolutionG-bandimages, obtainedwiththerecentlycommissionedRapidOscillationsintheSolarAtmosphere(ROSA) instrument, weresubjecttoanewMBP detectionalgorithm. AdistributionofMBP areawasfoundtobeconsistentwithlognormalstatistics, peakingsubstantiallyabovethediffractionlimitedresolutionofthetelescope. A sharpdropofffromthepeaktothediffractionlimitindicatesalowerlimitinarea, belowwhichMBPstendnottoexist.

Flaresandglobalwaves, includingseismicHughHudson (SSL/UC Berkeley)with

C.A. Lindsey, and J.C. Martinez-Oliveros

Solarflaresarecloselyassociatedwithlarge-scalewavesorotherglobalsignaturesinthecorona(typeII bursts, EIT waves, andCMEs), Globalwavesalsoappearinthechromosphere(Moreton),andintheinterior("sunquakes"). Themorphologyofthesephenomenasuggeststhatallbeginincompactsourcesatlowaltitudesinthesolaratmosphere, andthattheirexcitationiscloselyrelatedtotheimpulsivephaseoftheassociatedflare. Forthecoronalandchromosphericsignatures, theeffectscannotnowbeobservedclosetotheirradiantpoints. Theseismicsignatureismostconspicuous15-60Mmawayfromthesource, and30-60minutesaftertheimpulsivephase. Wediscussthemorphologyandenergeticsoftheseglobaleffects. Weshowthatthemagneticrestructuringinvolvedinflareenergyreleaseultimatelymustexciteeachofthethem. Thisprocessmayinvolveintermediarystepsthatareinmostcasesnotwellunderstood.

ThelinkbetweenSodiumintensityenhancementsandthephotosphericmagneticfield

DavidJess (Queen'sUniversityBelfast)withMihalis Mathioudakis, Damian Christian,

Philip Crockett, Sergiy Shelyag, andFrancis Keenan

IntensityenhancementsintheSodiumD1absorptionlineat5896Angstromsareoftenusedasaproxyforstrongunderlyingmagneticfieldconcentrations. Utilizingarangeofhigh-resolutionimagersandspectro-polarimeters, weshowhowthiscorrelationbreaksdownatlowmagneticfieldstrengths. Furthermore, weapplymulti-wavelengthanalysistorevealhowSodiumbrightpointsarerelatedtotheirG-band

counterpartsthroughthedetectionofhigh-velocitydowndraftsonsmallspatialscales.

Longitudinaloscillationsinanexpandinghotcoronalloop.

MarialejandraLuna (UniversityofSheffield)withR. Erdélyi, and G. Verth

Wavesandoscillationscanprovidevitalinformationabouttheinternalstructureofthewaveguidetheypropagatein. Hereweinvestigateanalyticallythemagnetohydrodynamic(MHD)longitudinalwavesinanexpandingcoronalloop.ItisouraimtounderstandwhathappenstotheMHD waveswhentheyaregeneratedinafluxtubewherethefluxtubehasanon-constant(e.g.expandingormagneticbottle)geometry. Thegoverningequationofthelongitudinalmodeisderivedintheapproximationofweakexpansionandissolvedundersomefurtherbyanalyticalapproximations(e.g. inthelimitofthethinfluxtubeapproximation, spatialandtemporalscaling,etc.). ItisfoundthatthepropagationofslowlongitudinalwavesinanexpandingmagneticfluxtubecanbedescribedbytheKlein-Gordonequation. Solutionintheformofhypergeometricfunctionsisdeterminedforthelongitudinaloscillations. Therelevanceofthesesolutionsforsolarmagneto-seismologywillbediscussed.

ExploitingtheCoronalSlowModeMikeMarsh (JeremiahHorrocksInstitute, UCLan)

with R.W. Walsh

Observationsofthethree-dimensionalpropagationofwaveswithinactiveregioncoronalloopsandameasurementofthetruecoronalslowmodespeedareobtainedusingSTEREO.Intensityoscillationsareobservedtopropagateoutwardfromthebaseofaloopsystem, consistentwiththeslowmagnetoacousticmode. ThewavephasevelocityismeasuredintheobservationsfromtheA andBspacecraft. Thesestereoscopicobservationsareusedtoinferthethree-dimensionalvelocityvectorofthewavepropagationandmagnitudeof132±9km/s, givingthefirstmeasurementofthetruecoronallongitudinalslowmodespeed, andaninferredtemperatureof0.84±0.12MK.TheseresultsareconfirmedusingHINODEspectroscopicobservations. Itisfoundthattheloophasauniformtemperatureprofilewithameantemperatureof0.89±0.09MK,inagreementwiththetemperaturedeterminedseismologicallyusingtheSTEREO observations.Theresultsfurtherstrengthentheslowmodeinterpretation, andimplythatitisnotpossibletodiscriminatebetweentheslowmodephasespeedandthesoundspeedwithintheprecisionofthepresentobservations.

PropertiesofMHD wavesinplasmawithvariablebackground

RichardMorton (UniversityofSheffield)withR. Erdélyi

Thesolaratmosphericplasmaisanextremelydynamicmediumthreadedbyacomplexmagneticfieldthatisconstantlysubjecttoheatingandcoolingprocesses. Themagneticfieldprovidesthefoundationsforawidevarietyofplasmafinestructureinthesolaratmosphere, e.g.coronalloops, coronalholes, prominences. Eachofthesefeaturesinthesolaratmospherecansupportanarrayofmagneto-hydrodynamic(MHD)oscillatorymodes. WepresenthereafirststudyofthepropagationofMHD wavesinamagnetisedplasmaenvironmentthatiscoolingduetoradiation. Previousinvestigationshave

60 P14

concentratedontheaffectofradiationontheperturbationsonly. AnapproximateradiationfunctionthathastheformofNewtoniancoolingisusedforthesakeofsimplicity. WefindthatthecoolingoftheplasmaleadstoatimedependentfrequencyofMHD waves(oroscillations)andcausesbothdampingandamplificationoftheseperiodicphenomena. Thisresultcouldhaveimportantimplicationsforvariousaspectsofmagneto-seismologyinthesolaratmosphere.

PhasemixingintheSolarCoronaBeniaminOrza (TheUniversityofSheffield)with

I. Ballai, and A. Marcu

TheproblemofphasemixingofsolarAlfvénwavesisrevisitedtakingintoaccountdissipativephenomenaspecificforthesolarcorona.OurestimationsshowthatthepreviousresultsderivedincontextoftorsionalAlfvénwavephasemixingareheavilyunderestimatedsophasemixingcannotbeusedtoexplainthedampingoftorsionalAlfvénwavesandheatingofopencoronalstructures. Wealsoshowthatinorderforthephasemixingtostillbeaviablemechanismunrealisticassumptionshavetobemade.

CoupledAlfvénandKinkOscillationsinCoronalLoops

DavidPascoe (UniversityofStAndrews)withA.N. Wright, and I. DeMoortel

Observationshaverevealedubiquitoustransversevelocityperturbationwavespropagatingoutwardinthesolarcorona. ToinvestigatethenatureoftransversewavespropagatinginthesolarcoronaandtheirpotentialforuseasacoronaldiagnosticinMHD seismology, weperformthree-dimensionalnumericalsimulationsoffootpoint-driventransversewaves. Weconsidertheeffectofstructuringontheirpropagationandbehaviour.Whendensitystructuringispresent, resonantabsorptionininhomogeneouslayersleadstothecouplingofthekinkmodetotheAlfvénmode.ThedecayofthepropagatingkinkwaveasenergyistransferredtothelocalAlfvénmodeisingoodagreementwithamodifiedinterpretationoftheanalysisofRuderman&Robertsforstandingkinkmodes. NumericalsimulationssupportthemostgeneralinterpretationoftheobservedlooposcillationsasacouplingofthekinkandAlfvénmodes. Thiscouplingmayaccountfortheobservedpredominanceofoutwardwavepowerinlongercoronalloopssincetheobserveddampinglengthiscomparabletoourestimatebasedonanassumptionofresonantabsorptionasthedampingmechanism.

Theeffectofdensitystratificationonthetransverseoscillationsoftwoparallelcoronal

loopsDavidRobertson (SheffieldUniversity)with

M.S. Ruderman, and Y. Taroyan

Transverseoscillationsofcoronalmagneticloopsareroutinelyobservedduringthespacemissions.Sincethefirstobservationtheseoscillationswereinterpretedintermsofkinkoscillationsofmagnetictubes. Sometimescollectiveoscillationsoftwoormorecoronalloopsareobserved. Thismakesthedevelopmentofatheoryofcollectiveoscillationsofseveralloopsadesirableone.Anotherreasonforthedevelopmentofthistheoryisthatthereareevidencesthatatleastsomecoronalloopsarenotmonolithicbutconsistofmanythinmagneticthreads. Herethelineartheoryofkinkoscillationsoftwoparallelmagnetictubeswiththedensityvaryingalongthetubesis

developed. Thissystemisusedtostudytheeffectofdensityvariationontheeigenfrequenciesofcollectiveoscillations.

AnatomyofaslowwaveinacoronalloopTomVanDoorsselaere (UniversityofWarwick)

with Nick Wardle, GiulioDel Zanna, andKishan Jansari

Weanalyseanobservationofa5minutequasi-periodicoscillationdetectedinthecoronallineFeXII at195A,nearthefootpointofacoronalloopinHinode/EIS dataon08Feb2007. Thesameoscillationisdetectedsimultaneouslyintwoothercoronallines, FeXIII at204A andFeXI at192A.Theoscillationisobservedforafull2periodsinbothDopplershiftandintensity. WeuseFourierandwaveletanalysistodeterminetheperiodoftheoscillationtobeP =314±83sintheDopplershiftandP =344±61sintheintensity. WeobservenegligiblephaseshiftbetweenDopplerandintensitytimeseries. Thisisstrongevidencefortheinterpretationoftheobservedphenomenonintermsofapropagatingslowmagneto-acousticMHD mode. Forthefirsttime, weusespectroscopytodetectoscillationsintheelectrondensity, usingtheCHIANTI atomicdatabase.ComparingthedensityvariationsandtheDopplershiftsallowsustoderivetheline-of-sightcomponentofthephasespeed. Thecomparisonofthetemperatureandthedensityallowstoestimatethecoronalvalueoftheratioofspecificheats.

MagnetoseismologyofthechromospherewithtorsionalAlfvénwavesGaryVerth (KU Leuven)

InspiredbythefirstdiscoveryofsolarchromospherictorsionalAlfvénwavesbyJessetal. (2009), magnetohydrodynamictheoryisdevelopedwhichpredictshowtheobservableproperties, e.g., frequency, amplitudeandvelocity, areevolvingwhilepropagatingthroughrealisticallystratifiedchromosphericwaveguides.ItisfoundthatthesespecialincompressiblemagneticwavescanbefullyexploitedasauniquemagnetoseismologicaltooltoprobetheplasmastructureoftheSun'sloweratmosphere, e.g.,offeringarealandpracticalmappingofthe3-Dmagnetismofthesolarchromosphere. Theproposedtechniquescanbeappliedtothelatesthighspatial/temporaldatafromtheUK fundedROSA (RapidOscillationsintheSolarAtmosphere)instrumentorthemuch-awaitedSDO(SolarDynamicsObservatory)satellite.

Evidenceofmagneto-acousticwavesinphotosphericobservationsofasunspot

SergeiZharkov (UniversityCollegeLondon–MSSL) with S. Shelyag, R. Erdélyi, and

M.J. Thompson

WeshowtheobservationalevidenceforthepresenceofMHD wavesinthesolarphotospherededucedfromSOHO MDI andHinodeobservations. Themagneto-acousticoscillationsareobservedasacousticpowerenhancementinthesunspotumbraathighfrequencybandsinthevelocitycomponenttransversetothemagneticfield. Weusenumericalmodellingofthewavepropagationthroughlocalisednon-uniformmagneticfieldconcentrationalongwiththesamefilteringprocedureasappliedtotheobservationstoidentifytheobservedwaves. Underpinnedbytheresultsofthenumericalsimulationsweclassifytheobservedoscillationsasmagneto-acousticwavespropagatingalongthefieldlineswithAlfvenspeedandexcitedbythetrappedsub-

photosphericacousticwaves. Weconsiderthepotentialapplicationofthepresentedmethodasadiagnostictoolformagnetohelioseismology.

P15A near-infraredstudyoftheMagellanicSystem

withVISTA.GemmaBagheri (UniversityofHertfordshire)with

Maria-Rosa Cioni

TheMagellanicSystemrepresentsthenearesttemplatetostudystellarpopulationsandgalaxyinteractions. Itcomprisesoffourcomponents: theLargeMagellanicCloud(LMC),theSmallMagellanicCloud(SMC),theMagellanicBridge(MB) andtheMagellanicStream(MS).

RecentmeasurementsofthepropermotionoftheMagellanicClouds(Kallivayaliletal. 2006)suggestforthefirsttimethatthesegalaxiesareapproachingtheMilkyWay, supportingthetidalformationoftheBridgefromanLMC,SMCinteraction.

TheBridgeandtheStreamarewelltracedbythedistributionofneutralhydrogen, butthereareveryfewobservationsthatinvestigatetheirstellarcontent. IntheBridge, youngstarshavebeenfoundbyIrwin(1991), Grondinetal(1992)andothers, buttodatenostarshavebeenobservedinthestream.

Thisprojectwillusenear-infraredobservationsfromtheliteraturetoinvestigatetheformationandevolutionoftheMagellanicSystem'stidalfeaturesincludingacontributiontotheVMC strategyfortheBridge. TheunprecedentedsensitivityoftheVMC datashouldalsoallowforthefuturediscoveryofstarsintheStreamaspredictedbyMastropietro(2009), withdynamicalmodelsoftheMagellanicSystem.

TheVMC survey- I.StrategyandEarlyScienceData

Maria-RosaCioni (UniversityofHertfordshire)withVMC Team

ThefirstobservingseasonoftheVMC surveyhasbeencompleted. ThesurveystrategywillbebrieflydescribedtogetherandthefirstscienceresultsontheLargeMagellanicCloudwillbepresented.

TheVISTA ScienceArchiveRossCollins (IfA,Edinburgh)with R. Blake,

N. Cross, N. Hambly, M. Holliman, R.G. Mann,M. Read, E. Sutorius, and P. Williams

ThisyearmarksthestartofVISTA'ssurveyoperationsandallofthedatafromtheseinfraredobservationsoftheSouthernHemispherearearchivedbytheUniversityofEdinburgh'sWide-FieldAstronomyGroup. Databasereleasesofthesourcecataloguesandobservationmetadatawillbemaderegularlyandafteraproprietaryperiodbecomeavailablepublicly. Theseareaccessibleon-lineviaawebinterface(http://surveys.roe.ac.uk/vsa)aswellasthroughthestandardinternationalvirtualobservatoryinterfaces. Herewedemonstratehowuserscanmakebestuseofthearchivedatabasedesigntoquicklyextracthigh-qualityscientificresultsfromtheavailabledataset.

P14–P15 61

FindingvariablesusingtheVISTA ScienceArchiveNicholasCross (IfA,Edinburgh)with

Nigel Hambly, Ross Collins, Eckhard Sutorius,Mike Read, and Rob Blake

TheVISTA VariablesinViaLactea(VVV) willreobserve500squaredegressoftheGalacticPlaneandBulgeoverthenextfewyearsin ∼ 100

separateepochstofindperiodicvariablestars,whichwillbeusedasdistanceindicatorsofthestructureswithintheMilkyWay. Thiswillleadtoadatasetof1billionuniquesources(withupto100billionsingleepochdetections)ontheskyofwhichtheremaybe1millionvariables. TheVISTAScienceArchivemustbeabletorobustlyfindandcategorisevariablessuchthatscientistscaneasilyselectspecifictypes.

UltraVISTAJamesDunlop (UniversityofEdinburgh)withKarina Caputi, and UltraVISTA consortium

UltraVistaisanew5-yearultra-deepnear-infraredsurveybeingundertakenwiththeVistasurveytelescopeintheCOSMOS extragalacticfield. BythetimeofthismeetingwewillhavebeguntoreceivedatafollowingcommencementoftheVistasurveysinFeb2010. I willsummarizethedesignofthissurvey, andreviewitspotentialforthestudyofhigh-redshiftgalaxyevolutioninthelightofrecentresultsfromHST andSubaru. I alsoplantodiscusstheperformanceofVistafordeepimaginginthelightofourfirstdata.

VISTA PerformanceJimEmerson (QueenMary, UnivofLondon)with

Will Sutherland

VISTA commissioningwascompletedinthe3rdquarteranditwashandedovertoESO inDecember2010. Theas-builtperformancewillbecomparedtotherequiremnts.

HighredshiftquasarsintheVIKING field.JosephFindlay (QMUL)

Theexistenceofluminousquasarsatz ∼ 6

suggeststhattheformationofthefirstsuper-massiveblackholesbeganwithinthefirstfewhundredmillionyearsofthebigbang. Assuch,high-zquasarsofferpowerfulprobesoftheearlyuniverse, allowingconstraintsonearlystructureformation, chemicalenrichmentandthestateoftheintergalacticmediumattheendoftheepochofcosmicreionization.

Attheforefrontofhigh-zquasarsearchesinthenextdecadewillbetheVISTA Kilo-degreeINfraredGalaxysurvey(VIKING).VIKING beganitscoverageofthesouthernskyinNovemberandshouldhavetherightcombinationofareaanddepthtodetect ∼ 10z > 6.5 quasarsoverits1500sq.degfootprint. UsingthelatestobservationaldataI willdiscussthepotentialtodetectandisolate6.5 < z < 7.5 quasarsovertheVIKING field, makingparticularreferencetocolourselectionstrategies, samplecontamination,efficiencyandcompleteness.

FirstobservationsofstellarclustersintheLMCfromtheVMC survey

RoaldGuandalini (UniversityofHertfordshire)with VMC Team

WepresentfewpreliminaryresultsonananalysisweareperformingonthestellarclustersintheLargeMagellanicCloudobtainedthankstothefirstobservationsmadebyVISTA fortheVMC

survey. Webuiltupasampleofstellarclustersconsideringonlytheoneslocatedinoneofthetilesmostobservedinthefirstmonthsofthecampaign. Weshownear-IR color-magnitudeplotsforfewofthemand, finally, weremindwhatarethescientificgoalsthattheVMC surveycouldreachontheirstudy.

TheVISTA DeepExtragalacticObservations(VIDEO) Survey

MattJarvis (UniversityofHertfordshire)withDave Bonfield, and VIDEO Consortium

I willpresentthemainsciencegoalsoftheVIDEOsurveyandprovideanupdateonthestateofthedataandanyearlyscienceresults.

TheVISTA sciencepipelineJamesLewis (InstituteofAstronomy)with

Mike Irwin, Simon Hodgkin, Eduardo Gonzalez-Solares, and Peter Bunclark

TheVISTA telescope, withaninfraredcameracomprising162K×2K Raytheondetectorsanda1.7squaredegreefieldofview, representsahugeleapininfraredsurveycapabilityinthesouthernhemisphere. Pipelineprocessingofinfrareddataisfarmoretechnicallychallengingthanforopticaldata. Infrareddetectorsareinherentlymoreunstable, whiletheskyemissionisuptoa1000timesbrighterthanmanyobjectsofinterest, andvariesinacomplexspatialandtemporalmanner.Tocompensateforthis, exposuretimesarekeptshort, leadingtohighnightlydatarates. VISTA willgenerate ∼ 0.25TB pernightoverthenext5-10years, whichexceedsthetotaldatarateofall8mclassterrestrialtelescopes.

InthispresentationwediscussthesciencepipelinethathasbeendevelopedtodealwithimagingdatafromVISTA anddiscusstheprimaryissuesinvolvedinanend-to-endsystemcapableof: robustlyremovinginstrumentandnightskysignatures; monitoringdataqualityandsystemintegrity; providingastrometricandphotometriccalibration; andgeneratingphotonnoise-limitedimagesandscience-qualityastronomicalcatalogues.

VISTA VariablesintheViaLactea(VVV) andnewUKIDSS GPS highamplitudeIR variables

PhilipLucas (UniversityofHertfordshire)withD Minnitti, M Hempel, V Ivanov, M Rekjuba, and

R Saito

I describetheVVV synopticsurveyoftheGalacticBulgeandtheGLIMPSE-SouthregionoftheGalacticplanewithVISTA.Thissurveyhasrecentlybegunandnotmuchdataarereducedyet. However, I presentsomeearlyUKIDSS GPSresultsonnewintriguinghighamplitudevariablestarsfromtwoepochK bandphotometryofseveraldozensquaredegreesoftheplane,separatedby3years. A largeproportionofthenewvariablesarelocatedinasinglestarformationcomplex, SerpensOB2, suggestingthattheyarepre-mainsequenceeruptivevariableswithunsteadyaccretion, similartotherareclassofFUOrionisstars. I discussthepotentiallyveryseriousimplicationsforthestellarbirthlineandtheHRdiagramsinpre-mainsequenceclusters.

TheVISTA HemisphereSurveyRichardMcMahon (UniversityofCambridge)with

VHS collaboration

TheVISTA HemisphereSurvey(V HS) willresultincoverageofthewholesoutherncelestial

hemispheretoadepth4magnitudesfainterthan2MASS/DENIS inatleasttwowavebandsJ andK.IntheSouthGalacticCap, 5000squaredegreeswillbeimageddeeper, includingH band, andwillhavesupplementaldeepmulti-bandgrizY imagingdataprovidedbytheDarkEnergySurvey(DES).TheremainderofthehighgalacticlatitudeskywillbeimagedinYJHK andcombinedwithugrizwavebandsfromtheVST ATLAS survey, SDSSBOSS andSkymapper. Themediumtermscientificgoalsinclude: ahugeexpansioninourknowledgeof; thelowest-massandneareststars; decipheringthemergerhistoryourownGalaxy; measurementoflarge-scalestructureouttoz=1andmeasuringthepropertiesofDarkEnergy; discoveryofthefirstquasarswith z > 7

VariableStarsintheVISTA near-infraredY,J,KssurveyoftheMagellanicCloudSystem(VMC)

MariaIdaMoretti (BolognaUniversity)withGisella Clementini, Maria-Rosa Cioni,Vincenzo Ripepi, Marcella Marconi,

Massimo Dall'Ora, Jean-Baptiste Marquette, andVMC Team

VMC,theVISTA Y,J,KssurveyoftheMagellanicClouds(MCs)willprovidethemeanK-bandmagnitude(outof12epochtime-seriesdata)forMC pulsatingvariablesforwhichperiodsarealreadyavailablefromopticalmulti-epochsurveys(OGLE,MACHO,andEROS II).

ThefirstVMC datawerecollectedstartinginNovember2009andcoversixLargeMagellanicCloud(LMC) fields: theGAIA SouthernEclipticPolecalibrationfield; thefamous30Doradusregion; twofieldsintheproximityoftheBridgeconnectingthetwoCloudsandtwofieldintheLMC outerdisk.

CombininginformationsfromtheEROS-II(Tisserandetal. 2009, A&A,501, 985)andtheOGLE-III (Soszynskietal. 2009, ActaAstronomica, 59, 1)catalogues, wehavecompiledthelistofRR LyraestarsexpectedtofallintothesesixLMC fields. ThevisualdatacovertheR,B andV photometricbands, whiletheVMC datawillprovidetheY,J,andKsmagnitudes.

StartingfromthefieldthatGAIA willobserveintheLMC,wewilllookfortheVMC infraredcounterpartsofknownvariablestars, willconstructtheirK-bandlightcurvesandderivetheirmeanK-bandmagnitudesandpulsationparameters. WewillthenconstructPL relationsintheK-band. FromthescatteronthesePL wewillinvestigateeffectsduetometallicity, ageandotherstellarparameters. BysearchingfordistancevariationswewillproducethefirstsystematicinvestigationofthestructureoftheLMC.

VIKING,theVISTA Kilo-degreeInfraredGalaxySurvey

WillSutherland (QueenMary, UniversityofLondon)with VIKING Team

I willdescribetheVIKING surveywhichhasrecentlystartedobservationsonthenewVISTAtelescopeatParanal, Chile. Thesurveyaimstocover1500deg2 ofextragalacticsky, overlappingwith2dFGRS andSDSS.VIKING willsurvey5bands, Z,Y,J,H,Ks, toapprox1.5magdeeperthantheUKIDSS LAS.EarlyfieldsarebeingtargetedontheHerschel-ATLAS regions. I willdescribetheearlydataprocessingandqualitycontrol, andoutlinethesciencegoalsofthesurvey.

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P16TheOVRO OphiuchusPre-Stellar(OOPS) Survey:

A 3.4mmContinuumEmissionStudyofCircumstellarMaterial

JoannaBulger (UniversityofExeter)withJ. Patience, H. Arce, S. Corder, J Koda,

J. Carpenter, and A. Sargent

Circumstellardisksarethebirthsitesofplanetformation. Bothdiskmassanddustopacityspectralindexarecrucialdiskparametersinunderstandingtheearlystagesoftheplanetformationprocess. Millimetercontinuumemissionprobestheopticallythin, coolerouterregionsofcircumstellardisksandisthewavelengthrangeatwhichthebulkofthecircumstellarmaterialemits.Theresultspresentedareofa3.4mmcontinuumsurveyusingtheOVRO interferometer, onasampleof34membersoftheRhoOphiuchimolecularcloud, oneofthenearestsitesofongoingclusteredstarformation. ThesampleconsistsofbothstarlessclumpsandClass0-IIyoungstellarobjects(YSOs), spanningtheevolutionarysequenceoflowmassstarformation.Theseobservationsinvestigatecircumstellarmaterialintheformofacircumstellardiskandsurroundingenvelope. Continuumemissionisdetectedin22ofthesourcesata3σlevel(typically0.9mJy), withatypicalbeamsizeof3’’.7×2”.3.ThemeasuredfluxesofthebrightestClass0andfaintestClassII objectsare; 227mJyand3mJyrespectively. Thedustopacityspectralindex,indicativeofgraingrowth, ofthesesourceshasbeendeterminedfromthesefluxmeasurements,takenincombinationwithpreviousmillimeterwavelengthobservationsobtainedfromtheliterature. Estimationsofthetotaldiskmassesofthesesourceshavebeendirectlycalculatedfromthemeasuredfluxdensities. Finally, themolecularlineemissionsof; HCN(1 − 0) (88.62679GHz),HCO+(1-0)(89.18858GHz)andCO(1 − 0)

(115.2712GHz), wereobservedsimultaneouslywiththecontinuumemissionandthedetectionsofwhichareusedastracersofsystemoutflow.

HighResolutionRadioObservationsofIRASFSC10214

RogerDeane (Oxford)with Steve Rawlings,Ian Heywood, Hans-Rainer Klockner, and

Richard Saunders

Thegravitationallylensed, starburst/AGNcompositegalaxyIRAS FSC10214hasbeenthetopicof > 100 publicationsoverthepast19years. ObservationsacrosstheEM spectrumfromX-raytoradiowavelengthsrevealpuzzlingandsometimescontradictoryfeatures. WereportthehithertounexploredhighspatialresolutionpropertiesofthisenigmaticobjectthroughMERLIN observations. Furthermore, wepresentthespectralenergydistributionwhichincludesnewobservationsat330MHz(GMRT),15GHz(RyleTelescope)andpreviouslyunpublishedSpitzerphotometry. WecomparetheinfraredSEDwithanensembleofgalaxieswithsimilarpropertiesfromtheObreschkowetal(2009)semi-analyticsimulationtoinvestigatetheeffectsofdifferentiallensingoftheAGN andstarburstcomponents.

Thespatialdistributionofcoldgasinhierarchicalgalaxyformationmodels

HansikKim (DurhamUniversity)with C.M. Baugh,A.J. Benson, S. Cole, C.S. Frenk, C.G. Lacey,

C. Power, and M. Schneider

Thedistributionofcoldgasindarkmatterhaloesisdrivenbykeyprocessesingalaxyformation: gascooling, galaxymergers, starformationandreheatingofgasbysupernovae. Wecomparethepredictionsoffourdifferentgalaxyformationmodelsforthespatialdistributionofcoldgas. Wefindthatsatellitegalaxiesmakelittlecontributiontotheabundanceorclusteringstrengthofcoldgasselectedsamples, andarefarlessimportantthantheyareinopticallyselectedsamples. Thehalooccupationdistributionfunctionofpresent-daycentralgalaxieswithcoldgasmass> 109h−2M⊙ ispeakedaroundahalomassof∼ 1011h−1M⊙, ascalethatissetbytheAGNsuppressionofgascooling. ThemodelpredictionsfortheprojectedcorrelationfunctionareingoodagreementwithmeasurementsfromtheHI ParkesAll-SkySurvey. WecomparetheeffectivevolumeofpossiblesurveyswiththeSquareKilometreArraywiththoseexpectedforaredshiftsurveyinthenear-infrared. Futureredshiftsurveysusingneutralhydrogenemissionwillbecompetitivewiththemostambitiousspectroscopicsurveysplannedinthenear-infrared.

OriginoftheCosmicRadioBackgroundAndyLawrence (UniversityofEdinburgh)with

S. Singal, L. Stawarsz, and V. Petrosian

A cosmicradiobackgroundseveraltimeslargerthananticipatedhasrecentlybeendetectedbytheARCADE experiment. Wereviewpossiblesourcesofthisbackgroundincludingtrulydiffuseemission, lowsurfacebrightnessradiogalaxies,andradiosupernovae, butconcludethatthebestexplanationisaverylargepopulationofveryfaintradiosources. Thishassignificantimplicationsforoneormoreoftheearlyhistoryofstarformation,theearlygrowthofblackholes, andtheconfusionlimitforSKA.

Thee-MERGE LegacySurveyTomMuxlow (JodrellBankCentreforAstrophysics)

with Ian Smail, Ian McHardy, and e-MERGEconsortium

e-MERGE isanambitiousLegacysurveytoexploite-MERLIN'suniquecombinationofsensitivityandspatialresolutiontostudytheformationandevolutionofstar-forminggalaxiesandAGN outtoredshiftsof z > 5. Theseobservationswillprovideapowerful, obscuration-independenttoolformeasuringthemassivestarformationandAGNactivityinhigh-redshiftgalaxies, hencetracingthedevelopmentofthestellarpopulationsandtheblackholegrowthinthefirstmassivegalaxies.Witharesolutionof50-200masinC- andL-Bands, correspondingto < 0.5 − 1.5 kpcatz > 1, e-MERLIN givesusourfirsttrulyreliableviewofthedistributionofstar-formationwithintypicalgalaxiesattheepochwherethebulkofthestarsinthepresent-dayUniversewerebeingformed. e-MERLIN willdisentangletherelativecontributionsofAGN andstar-formation, anessentialstepgiventheapparentlysimultaneousgrowthoftheblackholesandstellarpopulationsingalaxies. e-MERGE willalsostatisticallycharacterizethenatureofthesub-uJyradiopopulationwhicharethetargetobjectsfortheSKA.

Theluminosity-dependenthigh-redshiftcut-offoftheradioluminosityfunction

EmmaRigby (IfA Edinburgh)with Philip Best,Mairi Brookes, Jim Dunlop, John Peacock,

Louise Ker, Huub Rottgering, and Jasper Wall

Weuseanewmodel-independentmethodtoinvestigatetheevolutionofthesteepspectrumradioluminosityfunctionandquantifythehigh-redshiftcutoff. TheanalysisusestheCENSORSradiosourcesamplethatwehavedevelopedoverthepastfewyears, combinedwithadditionalradiodatafromtheWall&Peacock, ParkesSelectedRegions, HerculesandVLA COSMOS samples.Wefindconclusiveevidenceforaluminosity-dependenthighredshiftcut-offinthesteepspectrumradiosourcepopulation. Thespacedensityoflowerluminositysources(P1.4GHz = 1025 to 1026 W/Hz)peakatorbelowredshiftone, withshallowdeclinestohigherredshifts, whilstathighpowersthecutoffmovestohigherredshifts(z > 2 for P > 1027 W/Hz)andbecomesmorepronounced. Theexistenceofahighredshiftcutoffisconfirmedwithhighstatisticalsignificance, andisrobusttoestimatedredshifterrorsandtovariationsintheradiospectralindexwithredshift. WediscusstheimplicationsoftheseresultsformodellingtheradiosourcepopulationthatwillbeobservedathighredshiftsbytheSKA anditsprecursors.

P17LaboratoryStudiesofNon-thermalDesorptionof

AcetonitrilefromIcyGrainMantlesAliAbdulgalil (Heriot-WattUniversity)with

Elizabeth Hall, Lars Finger, Lisa Hodgson, andMartin McCoustra

Formationofmoleculesintheinterstellarmediumisamajorquestionwhichattractsconsiderableattention. ItwasthoughtthatthesmallmolecularprogenitorstoEarthwereformedthroughthegasphasereactionsintheatmosphereofouryoungplanet. Morerecently, ithasbeenproposedthatnon-thermalreactionsininterstellarandcometaryicescanproducetheseprogenitorspecies[1].Acetonitrile(CH3CN) isonesuchmoleculethatmightbetheprecursoroflargerbiogenicmoleculessuchasaminoacids. Ithasbeenobservedinanumberofgalacticenvironmentssuchas: acoldmolecularcloud(L134N);protostellarices(NGC7538:IRS9), protostellarhotcoregas(SgrB2(N));andinacometarycoma(Hale-Bopp)[2]. CH3CN islikelyformedontheicygrainsviagas-grainreactionsbetweenCH3andCN radicals. CH3CN normallydesorbstothegas-phaseattemperaturesnear90K,howeverdesorptioncanbeinducedbylowenergyelectrons[3]. Thispaperwilldiscusstheadsorptionofacetonitrileonmodelinterstellardustsurfacesandtheeffectofelectronirradiationofsuchadsorbedspecies.

References

1- W.D.Geppert, E.V., M.Hamberg, V.Zhaunerchyk, M.Kaminska, R.D.Thomas, F.Osterdahl, F.Hellberg, A.Ehlerding, M.Danielsson, andM.Larsson. Proc. IAU Symp.,2008, 251, 349. 2- S.B.Charnley, S.D.R., Y.J.Kuan, andH.C.Huang, Adv. SpaceRes., 2002,30, 1419. 3- A.Belloche, R.T.G., H.S.P.Müller,K.M.Menten, C.Comito, andP.Schilke, Astron.astrophys, 2009, 499, 215.

P16–P17 63

Thedeuteriumchemistryinlowandhighmassstarformingregions

ZainabAwad (Dept. ofPhysicsandAstronomy,UCL) with Serena Viti, and Estelle Bayet

Observationsofdeuteriumininterstellarmediumhavelongbeenusedtoprobethephysicalconditionswithininterstellarclouds. Observationsrevealthatdeuteratedspeciesareabundantoverawiderangeofastrophysicalregionsincludingwarmandhotcoresaroundlow-massandmassivestars, respectively. Earlymodelsattempttostudydeuteriumchemistryandexplainthehighobservedfractionationviagas-phaseschemes. Itisnowconfirmedthatgrainsurfacereactionsplayaroleinformingmanydeuteratedspecies. Inthisworkwefocusontheimportanceofaddingdeuteratedspeciestochemicalnetworksusedinastrochemicalmodelsandanalysetheirinfluenceontheabundancesofdifferentspecies, inparticularinhotcoreregions. Theinfluenceofchangingtheenvironments'physicalconditionsontheabundancesofthespeciesisalsoconsidered.

Extragalacticstarformationactivity- propertiesoftheverydensegas

EstelleBayet (UCL) with S. Viti, D.A. Williams,J. Martin-Pintado, and S. Martin

Toincreaseourcomprehensionofthestarformationmechanismsingalaxies, itisessentialtofirstbetterdeterminethepropertiesofthegaswhichformsstars. Unfortunately, whenobservingextragalacticstar-formationregions, ionised,neutral, diffuse, molecularandverydensegasareallwellmixedinsidethebeam. Onlyatreatmentmixingtheoretical(astrochemistryandastrophysics)andobservationalapproachescanhelpdisentanglethegascomponentsandthusincreaseourknowledgeonthemechanismsinvolved. Inaddition, onecouldasks: howdoestheenvironment(e.g. nuclearactivity)influencethepropertiesofthedustandgas? MytalkwillaimatpresentingthelatestresultswehaveobtainedinUCL onthetwosubjectsdescribedabove.

InvestigatingtheOnsetofSilicateCrystallizationintheEarlyStagesofStarFormation

SeanChapman (UniversityofManchester)withCiska Kemper

SpectrafromtheShort-WavelengthSpectrometer(SWS) oftheInfraredSpaceObservatory(ISO)obtainedfordeeplyembeddedmassiveYSOswillbeanalyzedandcomparedtothoseinthediffuseISM toinvestigatetheonsetofcrystallizationofsilicatesinmassiveYSOs. FeaturescharacteristicofthecrystallinespeciesforsteriteandenstatitearecommmonlyseeninemissionindisksaroundclassI/II YSOs. HerewefocusonmassiveYSOs,intheearlystagesofstarformation(e.g. Class0).Theseobjectsexhibitsilicateabsorptionfeaturesinthemid-infrared, whichprobethecircumstellarenvironmentandthemolecularcloud. Silicateshavebeenfoundincircumstellardisksaroundyoungstarswithtypicalcrystallinitiesof10-20%,whilstnocrystallinecomponenthasbeenobservedinthediffuseISM.Wehopetoprobethefirststagesofcrystallizationofinterstellarsilicates,afterthesegrainshaveleftthediffuseISM andhavebeenincorporatedintostar-formingmolecularclouds.

IsotopicFractionationinPrimitiveMaterial:QuantifyingtheContributionofInterstellar

Chemistry.StevenCharnley (NASA GoddardSpaceFlight

Center)

AnomalouslyfractionatedisotopicmaterialisfoundinmanyprimitiveSolarSystemobjects,suchasmeteoritesandcomets. Itisthought, insomecases, totraceinterstellarmatterthatwasincorporatedintotheSolarNebulawithoutundergoingsignificantprocessing. Wewillpresenttheresultsofmodelsofthenitrogen, oxygen, andcarbonfractionationchemistryindensemolecularclouds, particularlyincoreswheresubstantialfreeze-outofmoleculesontodusthasoccurred.Therangeoffractionationratiosexpectedindifferentinterstellarmoleculeswillbediscussedandcomparedtotheratiosmeasuredinmolecularclouds, cometsandmeteoriticmaterial. Thesemodelsmakeseveralpredictionsthatcanbetestedinthenearfuturebymolecularlineobservations, particularlywithALMA.

ChemistryofdenseclumpsnearmovingHerbig-Haroobjects

HelenChristie (UniversityCollegeLondon)

LocalisedregionsofenhancedemissionfromHCO+, NH3andotherspeciesnearHerbigHaroobjects(HHO's)havebeeninterpretedasarisinginaphotochemistrystimulatedbytheHHOradiationonhighdensityquiescentclumpsinmolecularclouds. Staticmodelsofthisprocesshavebeensuccessfulinaccountingforthevarietyofmolecularspeciesarisinginthephotochemistry, butthetimescaleofthephotochemistrydevelopmentisrathershort, soithasbeendifficulttoreconcilethemodelswiththeobservednumbersofemissionregions. Thechemicalmodelhasbeenadaptedtoincludeamovingradiationsource. Thisallowssomephotochemically-inducedspecies, includingmethanol, tomaintainhighabundancesformuchlongerthanthepreviousmodels.

FirstResultsfromSHINING - SurveywithHerscheloftheISM inNearbyINfraredGalaxies

NatalieChristopher (UniversityofOxford)withE. Sturm, A. Contursi, R. Genzel, J. GraciaCarpio,

S. Hailey-Dunsheath, D. Lutz, A. Poglitsch,L. Tacconi, J. DeJong, J. Fischer, A. Sternberg,A. Verma, S. Madden, M. Sauvage, L. Vigroux,Diane Cormier, U. Klaas, M. Nielbock, H. Linz,J. Schreiber, O. Krause, D. Lemke, E. Schinnerer,

F. Walter, and M. Haas

OnbehalfoftheSHINING consortium, I willoutlinetheSHINING surveyandpresentsomeofthefirstresultsfromdatatakenduringHerschel'sScienceDemonstrationPhase.

SHINING isaHerschelguaranteedtimekeyprogrammeofthePACS consortium. Itisacoherentfar-infraredspectroscopicandphotometricsurveyoflocalandintermediateredshiftinfraredbrightgalaxies(starbursts, AGN,(U)LIRGs, andlowmetallicitygalaxies). AnimportantfractionofstarformationandAGNactivityintheuniversetakesplaceinsuchdusty,infraredbrightgalaxies.

Ourgoalistousethesuperiorsensitivity, spatialandspectralresolutionofHerscheltostudythesegalaxiesinawavelengthrangethatisleastaffectedbyextinction. Weaimtoobtainacomprehensiveviewofthephysicalprocessesatworkintheinterstellarmediumoflocalgalaxiesrangingfromobjectswithmoderatelyenhancedstarformation

tothemostdense, energetic, andobscuredenvironmentsinultra-luminousinfraredgalaxiesandaroundAGN.TheSHINING samplecoversawideparameterrangeinluminosity, activitylevel,andmetalenrichment, andwillbecomplementedbyafewobjectsatintermediateredshifts, i.e. atamoreactiveepochofstarformation.

TowardsUnderstandingtheFormationofWaterintheInterstellarMedium

VictoriaFrankland (Heriot-WattUniversity)withMarkP. Collings, and MartinR.S. McCoustra

Exposedtotheharshradiationfieldsofinterstellarspace, fewmoleculescanescapephotodestruction. However, thevastcloudsofgasanddustthataccumulateinthegulfsofspacebetweenthestars(knownastheinterstellarmedium)havebeenobservedtocontainmorethan120differentmolecularspecies[1]. Thelowtemperature(10-100K) andpressure(10−14

mbar)conditionswithintheinterstellarmediumlimittherangeofviablegas-phasereactionsresultinginthegas-phasechemistryalonebeinginsufficienttoexplaintheobservedabundancesofsomekeychemicalspecies(forexample, H2, andH2O).Dustgrainsprovideasurfaceonwhichadsorbedspeciescanreact[2]andhenceanalternativepathwaytokeyinterstellarmolecules.ThemoleculeofinteresthereisO2. TherecentODIN andSWAS campaignshavedeterminedthegaseousO2abundancetobeconsiderablylowerthanthatoftheatomicO abundance[3]implyingthatO2maybeadsorbedontothegrain.

SurfacechemistrywithinanultrahighvacuumchamberisbeingusedtoexplorethedesorptionkineticsofO2onarangeofastrophysicallyrelevantsurfaces. Intheseexperiments, theproductsareidentifiedusingtemperatureprogrammeddesorptionandinterpretedusingkineticanalysisofasimplesurfacemechanism.TheultimateaimofthisresearchwillbetocombineatomicbeamsofO andH tostudyinsituH2O formationonagrainsurface.

References

[1]from“129reportedinterstellarandcircumstellarmolecules”http://www.cv.nrao.edu/%7Eawootten/allmols.html(assessed11December2008)[2]R.GouldandE.Salpeter, Astrophys. J., 1963, 138, 393[3]K.Acharyya, G.W.Fuchs, H.J.Fraser, E.F.vanDishoeckandH.Linnartz, A&A,2007, 466, 1005

AstrochemistryintheALMA eraGaryFuller (JodrellBankCentreforAstrophysics-

UK ALMA ARC)

ALMA willrevolutionizethestudyofastrochemistryinboththisandothergalaxies. InthispresentationI willpresentrecentinitialresultsfromtheJCMT SpectralLegacySurveytogetherwithrecentresultsfromastrochemicalmodels.ThesewillbeusedtohighlighthowALMA willimpactourunderstandingofastrochemistry, and,consequentlystarformation.

ChemicalevolutioninNGC 6302(theButterflynebula)

KerryHebden (JodrellBankCenterforAstrophysics)with Gary Fuller

Observationsofthebutterflyplanetarynebula(PN)NGC6302revealacomplexbi-polarstructurewithamassivelow-velocitytoruscoupledwithhigh-velocityknots. Thismassiveexpandingtorushasahighmass-lossrate(∼ 1.5 × 10−4M⊙yr−1;

64 P17

Trungetal, 2008)andisbelievedtocontainthehighestmassofcircumstellarmaterialofanyknownPN (between ∼ 1 to3M⊙; Perettoetal,2007). ItsstrikingmorphologyalsoconcealsaperculiarchemistrywherebybothOH maserandPAH emissionhavebeendetected.

Shocks, x-raysandanencroachinghardradiationfieldpermeatingNGC 6302aresimilarpropertiestothosefoundinAGN andaccordinglyprovideanextremeenvironmentinwhichtotestmodelsoftheinteractionofUV photonsandx-rayswithmoleculargas.

WereporthereonthefirstdetectionofCN,HCN,HCO+andatentativedetectionofSiC2towardsNGC 6302madeusingtheJamesClerkMaxwellTelescope(JCMT).Thesemolecularspecies, alongwithCO,aremodelledwiththeMeudonPDRcodetoconstrainconditionsinthesource. Theeffectsof12C/13C chemistryonmolecularabundancesarealsomodelledtoascertaintheiraffectsontherichchemistryinNGC 6302.

HotcoremodelsatlowmetallicityNadyaKunawicz (JodrellBankCentrefor

Astrophysics)with Gary Fuller, Estelle Bayet,David Tideswell, Andrew Markwick, and

Tom Millar

Hotcoresarethoughttobetheprogenitorsofmassivestarformation. InthispresentationI willdiscussthemodellingoftheisothermalcollapseofadarkcloud, andthefollowinghotcorestage. Thehotcoremodelisatimedependentchemicalmodel, whichusestheUMIST databaserate06reactionnetwork. Threemodelshavebeencreated, torepresenttheGalaxy, theLargeMagellanicCloudandtheSmallMagellanicCloud. ThemodelsusechemicalabundancestakenfromobservationsofHII regionsintheirrespectivegalaxy. Themodeloutputshavebeenusedtopredictcolumndensities. TheseresultshavebeenusedwithRADEX topredicttheobservablefluxseenacrossahotcoreforvariousspeciesincludingCS,HCN,HNC andHCO+. Theeffectofdecreasingmetallicityonanobservablehotcoreisthereforebeingexamined. TheresultsfromthisprojectshouldbedirectlycomparablewithALMA observationsofhotcoresinothergalaxies.

Photon- andElectron-drivenProcessesinModelInterstellarIces

MartinMcCoustra (Heriot-WattUniversity)

Modernsurfacesciencetechniquesallowustoprobeinequisitedetailtheinteractionofphotonsandelectronswithmodelsoftheicymantlesexpectedtogrowondustgrainsinthedenseinterstellarmedium. Thistalkwilldiscusstheresultsofmeasurementsonasimplemodelicecomprisingbenzene(C6H6)adsorbedonwatericesurfaces. Photonexcitationataround250nmandelectronexcitationaround250eV willbediscussed. Theimpactofthesemeasurementsonourunderstandingofthenon-thermaldesorptionoficygrainmantleswillbeoutlined.

TheXgearProject- A NewEraforAstrochemicalModelling?

PaulRuffle (JodrellBankCentreforAstrophysics)with Andrew Markwick(JBCA), Helen Roberts

(QUB),and Tom Millar(QUB)

XgearstartedlifeasawrapperprogrammewritteninC thatcollectedparametersforrunningastrochemicalmodelsusingtheHMC (hot

molecularcore)FortrancodebySteveRodgers(1998), assubstantiallydevelopedandupdatedbyHelenRoberts(2002onwards), whichutilisesLSODE:theLivermoreSolverforOrdinaryDifferentialEquations(Hindmarsh1983;RadhakrishnanandHindmarsh1993). ThegoaloftheXgearProjectistoenableastrochemicalmodelstoberuneasilyandconsistently, withfullusercontroloverthemanyparametersthatmustbespecifiedtorunamodel. Theseparameterscanbedefinedonthecommandlineand/orinaplaintextconfigurationfile. However, inthelongertermweintendtobuildaPHP-MySQL front-endtoXgear, sothatmodelscanalsobesetupandrunusingaclientwebinterfacetoa(remote)Xgearapplicationserverorcluster. Theresultsfromrunningsetsofmodelscoveringvariouspartsofparameterspacecouldthenbestoredinadatabaseforsubsequentquerying. OtherenhancementscouldincludealternativemodelenginestoHMC andtheinclusionofadditionalprocessessuchasgas-graininteractions. Initially,chemicalreactionrateswillbetakenfromUDFA2006: thenewUMIST databaseforastrochemistry(Woodall, Agundez, Markwick-KemperandMillar2006), whichreplacedRate99: TheUMISTdatabaseforastrochemistry(LeTeuffetal. 2000).ThecodeforXgearwillbemadepubliclyavailableunderthetermsoftheGNU GeneralPublicLicense. WeexpectthecodetocompilesuccessfullyunderLinux, UnixandOS X,forboth32- and64-bitplatforms.

P18Magnetospheric-periodoscillationsinSaturn'sequatorialmagnetosphereandopentaillobes

throughouttheCassinimissionDavidAndrews (UniversityofLeicester)with

S.W.H. Cowley, L. Lamy, and G. Provan

Wepresentnewresultsofanalysisofthenear-planetaryperiodoscillationsinSaturn'smagneticfield, employingallavailableCassinidataobtainedtodate, includingduringtherecentSaturnequinox. Inthisanalysisweuseanewfittothepreviouslystudiedspatialvariationsinthephaseoftheseoscillations, anddeducesecularchangesintheirperiodicities. Pre-equinoxtheseequatorialmagneticfieldoscillationsarefoundtobeconsistentlyinphasewiththoseobservedonSouthern-hemisphereopenfieldlines, andhencewiththedominantcomponentoftheSaturnkilometricradiation(SKR) emission. Meanwhile,fieldoscillationsonopenfieldlinesintheplanet'sNorthernhemisphereareconsistentlyfoundtobeinphasewiththeweaker, longer-periodcomponentoftheSKR.Nearequinox, wehavenowobservedarapiddecreaseintheperiodoftheequatorialfieldoscillations. Consequencesofthesenewfindingsarediscussed.

InterpolationofexternalmagneticfieldsoverlargesparsearraysusingSphericalElementary

CurrentSystemsCiaranBeggan (BritishGeologicalSurvey)with

Sam McLay

Interpolationofthemagneticfielddisturbancestoapointremotefromanobservatorycanbeachievedbyemployingthelatitudinal-weightedarithmeticmeanofthefieldasmeasuredattwoobservatories, onetothenorthandonetothesouthofthepointofinterest. Analternativetechniqueforinterpolatingexternalmagneticfield

disturbancesacrosslargespatialareascanbeachievedwiththeSphericalElementaryCurrentSystem(SECS) methodusingdatafromground-basedmagneticobservatories. TheSECS methodrepresentscomplexelectricalcurrentsystemsasasimplesetofequivalentcurrentsplacedataspecificheightintheionosphere. Themagneticfieldrecordedatobservatoriescanbeusedtoinvertfortheelectricalcurrentsandsubsequentlyusedtointerpolateorextrapolatethemagneticfieldacrossalargearea. Weshowthatinvertingforinducedsubsurfacecurrentsystemsinadditiontoionosphericcurrentsystemscanresultinstrongimprovementstotheestimateofinterpolatedmagneticfield, particularlyintheradialcomponentofthefield. Wedemonstratethatrelativelyfewobservatoriesarerequiredtoproduceanestimatewhichisbetterthanthenullhypothesis(i.e. assumingnochangeinthefield)orinterpolationusinglatitudinalweightingofdatafromotherobservatories. WefurtherinvestigatetheapplicationoftheSECS methodinmid- tohighgeomagneticlatitudesusingaseriesofobservatorynetworkstotesthowwelltheexternalfieldcanbeinterpolatedoverlargedistances.

AnestimationoftheCarringtonflaremagnitudefromsolarflareeffects(sfe)inthegeomagnetic

recordsEllenClarke (BritishGeologicalSurvey)with

Craig Rodger(UniversityofOtago), Mark Clilverd(BAS), Thomas Humphries(BGS), Orsolya Baillie

(BGS),and andAlan Thomson(BGS)

InthisstudywereviewpreviousworktoestimatethemagnitudeoftheCarringtonsolarflare(1September1859)andre-examineobservationsofsolarflareeffects(sfe)ontheKewandGreenwichObservatorymagnetograms. A databaseofmorerecenteventsisconstructedfrom: existingsfedataavailableon-line; magneticobservatoryyearbooks; sfedatacollectedandprocessedbyEbroObservatory; additionalscalingofeventsusingone-minutevaluesfromvariousINTERMAGNET andWDC magneticobservatories; andGOES X-rayfluxdata. WeinvestigatefourofthelargesteventsindetailandalsothestatisticalrelationshipbetweensfemagnitudeandX-rayfluxwithrespecttosolarzenithangleandgeomagneticlatitudeandusetheresultstoestimatethesizeoftheCarringtonflare.

EstimatingtheExtremesinGeomagneticActivityAcrossEurope

EwanDawson (BritishGeologicalSurvey)withAlanP Thomson, and Sarah Reay

Rapidlychanginggeomagneticfieldvariationsconstituteanaturalhazard, forexampleinnavigationand, throughgeomagneticallyinducedcurrents, topowergridsandpipelinenetworks.Thecontinuousmagneticmeasurementsavailabletohelpusunderstandthishazardtypicallyextendbacklessthan100years; thisproblemofthelackofalong-termdatasetiscompoundedbythefactthatmuchoftheolderdataisalsoinanalogueform, orisonlyavailabledigitallyashourlyordailymagneticindicesormeanlevels. So, itmaynotyetbeclearwhatthetrueextremesingeomagneticvariationsare, particularlyatthetimescalesofsecondstominutesthatarerelevantforestimatingthehazardtotechnologicalsystems.

Wethereforepresentananalysisbasedontheapplicationofastatisticaltechnique- 'extremevaluetheory'- toanumberofdecadesofoneminutesamplesofmagneticdatafromobservatoriesacrossEurope, andexplore

P17–P18 65

estimatedmaximainfieldvariationsinthehorizontalstrengthanddeclinationofthefield.Thesemaximaareexpressedintermsofthegreatestmaximumthatmaybeobservedonceevery100and200years. Wealsoexaminetheextremesintheone-minuterateofchangeofthesefieldcomponentsonsimilartimescales.

Theresultsshouldfindapplicationinbothhazardassessmentandinnavigationapplications. Theresultscanalsobeusedtomorerigorouslyanswertheoften-askedquestion: "justhowlargecangeomagneticvariationsget?

SpritesandRelativisticElectronBeamsAboveThunderclouds

MartinFullekrug (UniversityofBath)withToby Whitley, and Michael Rycroft

Ithasrecentlybeendiscoveredthatparticularlyintenselightningdischargescangeneratespritesandsubsequentlyupward-directedrelativisticelectronbeamsabovethunderclouds. Thisextendsthephenomenonofrelativisticrunawaybreakdownbelievedtooccurinsidethundercloudstotheatmosphereabovethunderclouds. Thismarksaprofoundadvanceinourunderstandingoftheatmospherebecausewenowknowitactsasagiant, natural, particleaccelerator. TheacceleratedelectronscanreachsignificantrelativisticenergiesofsomeMeVduringtheirpassagefromthetroposphere, throughthemiddleatmosphere, intonear-Earthspace.Theserelativisticelectronbeamsconstituteacurrentabovethundercloudsandeffectivelytransferenergyfromthetropospheretothemiddleatmosphere. Thiscouplingprocesstherebyformsanovelelementoftheglobalatmosphericelectriccircuitwhichlinkstroposphericthundercloudstotheatmosphereabove.

SuperDARN observationsofthesub-auroralconvectionresponsetoenhancedgeomagnetic

activityAdrianGrocott (UniversityofLeicester)with

M. Lester, S.E. Milan, and T.K. Yeoman

A recentadditiontotheSuperDualAuroralRadarNetwork(SuperDARN),theBlackstoneradarislocatedat ∼ 50 degreesmagneticnorth, ∼ 10

degreesequatorwardofitsauroralcounterparts. Atthislatitudetheradarregularlymakesobservationsofplasmaconvectionequatorwardofthemainauroraloval. Theseobservationsreveallowvelocitysub-auroralionosphericscatterthatiswellcorrelatedwithboththeringcurrent(SYM-H)andauroralelectrojet(AE) indicesindicatingitisrespondingdirectlytogeomagneticactivity. Inthispaperwepresentsomestatisticalverificationofthisrelationship, andinvestigatethetimedelaybetweentheauroralenhancementsandthesub-auroralconvectionresponse. Inaddition, wepresentsomenear-conjugateTHEMIS observationsofamagnetosphericsubstormwhichsuggestadirectrelationshipbetweenlocalisedsubstormactivityandtheobservedsub-auroraldynamics.

ObservationsofGeomagneticStormsoveraSolarCycle: SomeInitialFindings

JamesHutchinson (UniversityofLeicester)withD.M. Wright, and S.E. Milan

Geomagneticstorms, periodsofintensesolarwind–magnetospherecouplingusuallyassociatedwithextremeconditionsinthesolarwindsuchascoronalmassejections(CMEs)orco-rotatinginteractionregions(CIRs), causelargeglobaldisturbancesintheEarth’smagnetosphere;

depositinglargeamountsofenergyintothemagnetotailandproducinganenhancedringcurrentandenergisingplasmatorelativisticlevels,throughyetunknownexcitationmechanisms.

ByexploitingdatafromtheAdvancedCompositionExplorer(ACE) spacecraftinconjunctionwithspace- andground-basedmeasurementsatEarthoverthelastsolarcycle, adatabaseofgeomagneticstormshasbeencompiledandanalysed. Herewepresentsomeinitialstatisticalfindingsfromasuperposedepochanalysisof157eventsidentifiedfromtheglobalSYM-H index. Diurnalvariationinstormactivityisobserved, alongwiththegeneraltrendofactivityoverthesolarcycle. RadarmeasurementsfromtheSuperDARN andauroralimagesfromthefar-ultraviolet(FUV) packageonboardtheIMAGEsatelliteandtheultravioletimager(UVI) onboardthePolarspacecraft, arealsopresentedusinganewradarbeamkeogramtechniquetodemonstratevariationsintheauroralovalduringstormconditions. Theresultsofcorrelationstudiesbetweenstormsizesandsolarwindinputthroughcommoncouplingfunctionswillalsobediscussed.

OverviewoflowenergyelectronobservationsinthevicinityofSaturn'smoonEnceladus

SheilaKanani (UniversityCollegeLondon–MSSL)with Geraint Jones, Gethyn Lewis, Chris Arridge,

Andrew Coates, and Dave Young

EnceladusresidesdeepwithinSaturn'smagnetosphere. Themagnetosphericplasmaincidentonthesatelliteisabsorbed, formingathermalplasmawakedownstreamofthemoon,andacavityinhigherenergypopulations. WhentheCassinispacecraftcrossesEnceladus'sL-shell,thesecavitiesareobservedasbriefdropoutsinenergeticparticlefluxes, ormicrosignatures, mostclearlyobservedbytheMagnetosphericImagingInstrument(MIMI).A surveyofthermalplasmaobservationsbytheCassiniPlasmaSpectrometer(CAPS) instrumenthasrevealedtheexistenceofvariousfeaturesinlowenergyelectronsclosetothetimesofmicrosignatures, orimmediatelybeforeoraftertheiroccurrence. Thesefeaturesvary; somepresentthemselvesasasetofdiscretespikes, coveringelectronenergiesof9-15eV andlasting, intermittently, uptotensofminutes. Othershowevidenceofinjectioneventsclosetothemoon'sorbitalplane. Wepresenttheresultsofasurveyoftheseperplexingfeatures, suggestpossiblecausesfortheiroccurrenceanddiscussresultsfromcloseEnceladusflybys.

NatureoftheringcurrentinSaturn’sdaysidemagnetosphere

StephanieKellett (UniversityofLeicester)withC.S. Arridge, E.J. Bunce, A.J. Coates,

S.W.H. Cowley, M.K. Dougherty, A.M. Persoon,N. Sergis, and R.J. Wilson

DeterminationofthephysicalnatureofSaturn'sringcurrent, i.e., theactualcombinationofcurrentsassociatedwiththeinertiaofthenear-corotatingplasmaandhotparticleeffects, hasbeenthesubjectofmuchdebateforalmost30years.

HereweinvestigatethenatureoftheringcurrentinSaturn’sdaysidemagnetosphereusingmagneticfield(MAG) andplasmaparticle(CAPS,MIMI andRPWS) datafromtwotypicalnear-equatorialpassesoftheCassinispacecraftspanningtheradialrangebetween ∼ 3 and ∼ 20RS (RS isSaturn'sequatorialradius, equalto60268km). Physically,

theplasmacurrentsthatformtheringcurrentareduetooneormoreofthreepossibleeffects; thespatialgradientoftheperpendicularplasmapressure, theanisotropyoftheplasmapressuresparallelandperpendiculartothefieldlines, andtheinertiaoftheflowing(near-corotating)plasma.WeexamineplasmaparametersobtainedbyCassiniforeachpassandcomparetheazimuthalcurrentdensityprofilesdeducedwiththoseobtainedfromcurrentdiskmodelingofthemagneticfieldperturbations.

WeshowthatthecurrentassociatedwiththePperp > Ppara pressureanisotropyofthewarmwatergroupionsisimportantinside ∼ 10RS ,cancellingasignificantfractionoftheotherwisedominantinertiacurrentinside ∼ 6RS . Theoveralltotalcurrentdensityprofileisthenfoundtobesimilartothatproducedbythepressuregradientcurrent, butaugmentedinstrengthbyfactorsof ∼ 1.5 − 2.0 bythedifferencebetweentheinertiaandanisotropycurrents. Thededucedcurrentdensityprofilesareingoodagreementwiththegrossfeaturesoftheprofilesdeducedfromcurrentdiskmodeling, thoughwiththecurrentdensitythenfallingmoresteeplywithradialdistancethanthe 1/r dependenceassumedinthemodel.

Towardsmodellingofhighlatitudemagneticfieldsfromsatellitedata

GemmaKelly (UniversityofLiverpool)withRichard Holme, and Alan Thomson

Recentlow-Earthorbitsatellitemissionshaveprovidedawealthofhighqualitydataallowingforimprovedmodelsofthenear-Earthgeomagneticfield. However, understandinginthehighlatituderegionsislaggingbehindduetothecomplexityoftheprocessesandinteractionsinthisregion. Weinvestigateresidualsbetweensomerecentmodels(CHAOS-2, T01andCM4)anddatafromtheCHAMP andØrstedsatellites, withtheaimofinvestigatinghowwellthemodelsfitthedata,particularlyregardingthehighlatituderegions.

Bylookingattheresidualsonanorbit-by-orbitbasiswehaveshownthatallthreemodelsshowverysimilarfeaturesintheresiduals. Wecanidentifycurrentsourcesthatareconsistentintimeandco-latitude, evenatveryquiettimes(Kp < 2o,night-sideonly). ThereisalsosomecorrelationbetweenthesizeoftheresidualsandlevelofactivityindicatedbythePC andAE indices. Wheninvestigatingtwo-dayaveragedresidualplotstheauroralovalcanbeidentified, andthereareenhancedresidualsoverthepolarcaps, forbothquietanddisturbedtimes. Thisinformationwillbefedintoamethodforimprovinggeomagneticfieldmodelsathighlatitudes.

CoordinatedgroundandspaceobservationsofGeospace: A viewfromthegroundMarkLester (UniversityofLeicester)

Thestudyofthesolarwindmagnetosphereionospheresystem, sometimesreferredtoasGeospace, isbestconductedbybringingtogetherarangeofobservationaltools. Specifically, itisimportanttounderstandthatbothinsitumeasurementsbyspacecraftandremotesensingofmeasurementsbyspacecraftandfromthegroundprovideanincomparabledatasetforsuchinvestigations. Inthelastdecadeorso, spacemissionssuchasCluster, ThemisandIMAGE,havebeenaugmentedbyarangeofgroundbasedsystems, suchascoherentandincoherentscatterradars, magnetometers, riometersandauroralcamerasandspectrographs. Herewepresentan

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overviewoftheimportanceofcoordinatedgroundandspaceobservationsinordertodevelopourunderstandingofthelargerGeospacesystem. Weillustratethiswithexampleswhicharetakenfromavarietyofinstrumentsandstudies, whichillustratethecomplexity, bothintimeandspace,ofthesystemwhichweareinvestigating. WealsonotetheopportunitiesthatexistforcontinuedexplorationofGeospacewiththecurrentandfuturemissionsandinstrumentsaswellasbythecombinationofdatasetsinnovelways.

GPS PlasmsphericimagingCathrynMitchell (UniversityofBath)with

P Spencer

ThispaperoutlinesamathematicalapproachtoimagingtheelectrondensitydistributioninthelowerplasmasphereusingGPS measurementsfromlowEarthorbit(LEO) satellites. Theproblemofionosphericimagingusingground-basedGPSmeasurementshasbeenstudiedforanumberofyears. Suchmethodshaveprovedextremelyusefulinprovidingdetailsofthelargerscalemorphologyoftheglobalionosphere. TheworkpresentedextendsthesemethodssoastobeabletoimagetheplasmasphereuptoaltitudesoftheGPSsatellitesat20000km. TheproblemoflimitedobservationsduetothesmallnumberofLEO’sinoperationisovercomebyconstrainingtheplasmasphericelectrondensitytobeconstantalongmagneticfieldlines. ItisshownthatacoordinatetransformfromasphericalcoordinatesystemtoonedefinedintermsofEulerpotentialsissufficienttoprovideunambiguoussolutions.PreliminaryresultsusingdatafromtheCOSMICsatelliteconstellationarepresentedshowingtheresponseoftheplasmaspheretochangesintheinterplanetarymedium.

TheresultsclearlyshowtheresponseoftheplasmaspheretochangesintheIMF magneticfieldareconsistentwithreportedobservationsfromotherauthorsusingindependentobservationtechniques. PotentialnewscientificinvestigationsintomajorstormswillbepossiblewhenGPS datafromtheforthcomingSWARM missionareavailableandtheseideasarediscussed.

Evidencefortheoccurrenceof 10.6hmagneticfieldoscillationsinSaturn’sequatorial

magnetosphereGabbyProvan (UniversityofLeicester)with

D.J. Andrews, S.W.H. Cowley, M.K. Dougherty,and L. Lamy

Andrewsetal. (2008)andProvanetal. (2009)reportedCassiniobservationsofnear-planetaryperiodmagneticfieldoscillationsinSaturn’snear-equatorialmagnetosphere, andshowedthattheirperiodwascloselysimilartotheslowly-varyingperiodof ∼ 10.8 hdeterminedbyKurthetal.(2008)frommodulationsofSKR radioemissions.Kurth. etal(2008)furtherreportedthattheseemissionsalsoexhibitedasecondperiodof∼ 10.6 h. FurtherinvestigationbyGurnettetal.(2009)revealedthatthe ∼ 10.6 hmodulatedemissionoriginatesfromtheNorthernhemisphere,whilstthe ∼ 10.8 hmodulatedemissionoriginatesfromtheSouthernhemisphere.Andrewsetal. (2008)andProvanetal. (2009)alsofoundsignificant‘jitter’inthephasesoftheequatorialoscillations, andpresentedevidencethatmuchofthisisnotduetomeasurementerrorsbuthasarealphysicalcause. Hereweshowthatthisphase‘jitter’isduetothesuperpositionintheequatorialmagnetosphereoffieldoscillationsattheSouthernperiodwithweakeroscillationsatthe

Northernperiod. Wedeterminetherelativeamplitudesoftheseoscillations, andthephaseoftheNorthernperiodoscillationsrelativetotheNorthernSKR modulation.

ObservationsandmodellingofartificialD-regionheatingseenbyARIES

AndrewSenior (LancasterUniversity)withM.J. Kosch, and F. Honary

ArtificialradiowaveheatingofelectronsintheD-regionisusedasadiagnostictechniqueforstudyingpolarmesosphericsummerechoes, aradarphenomenoncausedbyminuteiceparticlesinthevicinityofthemesopause. Recentstudiesoftheheatingusingthecross-modulationtechniquefoundthatmodelsusedtopredicttheheatingoverestimatedtheobservedcross-modulationbyafactorof1.5-2.5. TheAdvancedRio-ImagingExperimentinScandinavia(ARIES),ahigh-resolutionimagingriometersystem, observedchangesintheionosphericabsorptionofcosmicradionoiseduringD-regionheating. Theseobservationshavebeencomparedtopredictionsfromasimilarmodeltothatusedwhenanalysingthecross-modulationresults. Provisionalresultsshowthatthemodeloverestimatesthechangeincosmicnoiseabsorptionbyafactorofabout2.TheseresultsleadustoquestionthevalidityoftheusualmodelsofD-regionheatingbypowerfulHFradiowaves.

SCANDI:All-skyviewofmeso-scalespatialstructureinthethermosphereandion-neutral

couplingoverSvalbardTimothySpain (UCL) with A.L. Aruliah,H.-C.I. Yiu, I. McWhirter, E.M. Griffin,

A. Charalambous, M. Kosch, L. Baddeley,V.S.C. HowelI,and I. McCrea

TheUCL ScanningDopplerImager(SCANDI) isanall-skyFabry-PerotInterferometerthatislocatedattheKjellHenriksenObservatoryonSvalbardneartheEISCAT ESR radars. Itprovidesroutinenighttimeobservationsofthetwomostprominentauroralandairglowemissionsat630nmor557.7nm. Theseallowmeasurementsofthermosphericwinds, temperaturesandintensitiesataround240kmand120kmaltitude, whichroughlycorrespondtotheF- andE-regionionosphere. Itisoneof3existingSDIsintheworld; theothertwoaretheoriginalAlaskanSDIandMawson, AntarcticaSDI.RecentlythefirstconjugatestudyoftheupperthermospherewasmadebycomparingtheSCANDI withtheMawsonSDI.Theseinstrumentshaveupsetthestandardassumptionsofaslowlyvaryingthermosphere.EISCAT-SCANDI experimentsusinghightemporalandspatialresolutionmeasurementshaveshownlocalisedrapidresponsestoionosphericvariability(10sofminutesoverafewhundredkilometreshorizontaldistance), butalsoanunderlyinginertia.Theeffectsofthisbehaviourappearinunexpectedamountsofheatingandaccelerationoftheupperatmosphere, andhaveconsequencesforfeedbackmechanismsthroughtheneutralwinddynamo.

Observationsofdouble-peakedHF radarspectraduetomixedechoesfromnaturalandartificial

plasmairregularitiesHannahVickers (UniversityofLeicester)with

Terry Robinson

CUTLASS HF backscattertargetsmaybeartificiallyinducedthroughtheuseoftheEISCAT highpowerionosphericheatingfacilityatTromsø, NorthernNorway. Plasmairregularitiescreatedinthiswayareknowntobehighlyfield-alignedandusually

possesslowspectralwidth. Inthevicinityofnaturalwavesandirregularitiesundermoredisturbedgeophysicalconditionshowever, thespectralwidthofartificialirregularitiesasdeducedbythestandardSuperDARN ‘FITACF’analysis, canbesometimesappeartobebroadened. Inthiswork, wepresentsuchobservationsandemploytheBurgmaximumentropyanalysismethodtoCUTLASS HF radarspectra, combinedwithstandard‘FITACF’parametersandDMSP satellitemeasurementstoshowhowmixedartificialandnaturalHF echoesfromspatiallyseparatedsourcescangiverisetodouble-peakedspectraasaresultofdetectionattheedgesofantennamainlobe

Presentdaychallengesinunderstandingthegeomagnetichazardtonationalpowergrids

JimWild (LancasterUniversity)withA.W.P. Thomson, C.T. Gaunt, P. Cilliers,B. Opperman, L.-A. McKinnell, P. Kotze,

C.M. Ngwira, and S.I. Lotz

Solaractivitygivesrisetochangesinthenear-Earthspaceenvironment, oftenreferredtoasspaceweather, thatcanadverselyaffecttechnologiesonandabovethesurfaceoftheEarth. Forexample, theimpactofacoronalmassejectionontheEarth’sprotectivemagnetospherecanleadtoageomagneticstorm, boostingexistingmagnetosphericcurrents. ThesecurrentsystemscauselargemagneticvariationsthatinduceelectricfieldsinthesolidEarth. Thesefields, inturn, generategeomagneticallyinducedcurrentsthatflowinconductingpipesandwires, inwaysinfluencedbytheelectricalpropertiesofeachnetwork. Consequently, powergridsandpipelinenetworksatalllatitudesareatriskfromthenaturalhazardofGICs. Assolaractivitybeginstoincreasefromthedeepestsolarminimuminacentury, weconsiderthecurrentunderstandingofthishazard,asitaffectsmajorpowersystemsinEuropeandAfrica. Wealsosummarisewhatcanbesaidwithsomecertaintyaboutthehazardandwhatresearchisyetrequiredtoaddressoutstandingquestionsanddevelopusefultoolsforgeomagnetichazardmitigation.

TrackingsolarwindstructuresfromtheSunthroughtotheorbitofMars

AnthonyWilliams (UniversityofLeicester)withN.J.T. Edberg, S.E. Milan, M. Lester, and M. Franz

WithnodirectupstreammonitorsofthesolarwindateitherVenusorMars, thesolarwindinputstotheplasmaenvironmentsofbothplanetsmustbeinferred. Wepresentamethod, usingacombinationofimagesfromtheHeliosphericImagers(HI) ontheSolarTerrestrialRelationsObservatory(STEREO) andin-situmeasurementsfromtheAdvancedCompositionExplorer(ACE)situatedatEarth’sL1pointtotracktheprogressionofCorotatingInteractionRegionsthroughtheinnerheliosphere, andtopredicttheirarrivalatVenusandMars. Weshowtheresultsofthismethodforsolarminimumfrom1July2007to31July2008, demonstratingthatthereisgoodagreementbetweenexpectedarrivaltimesandobservedenhancedactivityateachplanet.

Comparisonsofplasmatransportinthehigh-latitudeionospheresoftheEarthandVenus.

AlanWood (AberystwythUniversity)withS.E. Pryse, M. Grande, and H.R. Middleton

ThepresenceofaplanetarymagneticfieldatEarthandtheabsenceofsuchafieldatVenusresultsinsubstantialdifferencesinthedynamicsandmorphologyofthehigh-latitudeionospheres. In

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bothcasesphotoionisationistheprimarymechanismbywhichthedaysideionosphereiscreatedwhileparticleprecipitationandtransportprocessesacttomaintaintheplasmadensitiesatnight. HoweverthemechanismsdrivingplasmatransportatEarthandVenusarefundamentallydifferent.

ResultsarepresentedfromtheterrestrialionosphereduringintervalswhentheIMF isnorthwardwhichshowthattheTongue-of-Ionisation(TOI) canbedrawnaroundtheperipheryofthepolarcap(Middletonetal., 2005)andintothenightsideionosphere(Woodetal.,2008). Inthemagneticmidnightsectorsubstormscanmodulatethehigh-latitudeconvectionpatternandhencealterthespatialdistributionoftheplasma(Woodetal., 2009). WhenthesolarterminatorislocatedinthemagneticmidnightsectorpolarcappatchescanformbythebreakupofaTOI duetovariationinthehigh-latitudeconvectionpatterndrivenbythechangesintheIMF (WoodandPryse, inpreparation). Plasmastructuresinthissectoralsoshowaclearseasonalvariationduetochangesinthethermospherewiththeratioofthepatchdensitytothatofthesurroundingionospherebeinggreaterinwinterthansummer(WoodandPryse, 2009).

AtVenusobservationsofionsathighlatitudesclosetothesolarterminatorshowasymmetriesinboththedawn-duskandnoon-midnightplanes.Theseresultsshow, forthefirsttime, thepresenceofanightwardionflowatsolarminimum. Thevelocityofthisflowincreaseswithaltitudeanditislikelytocontributetothelossofionsfromtheplanettothesolarwind(Woodetal., inpreparation).

CombiningincoherentscatterradardataandIRI2007tomonitortheopen-closedfieldline

boundaryduringsubstorms.EmmaWoodfield (LancasterUniversity)with

J.A. Wild, A. Senior, and A.J. Kavanagh

Thesizeofthepolarcap, andhencetheamountofopenmagneticfluxcontainedwithinit, isaveryimportantquantitywhenitcomestounderstandingthesubstormprocessaswellasreconnectionratesingeneral. Ground-basedproxiesoftheopen-closedfieldlineboundary(OCFLB) havethereforebeenofgreatinterestinrecentyears. InthisworkwebuildonpreviousstudiesbyAikioetal(e.g. Ann. Geophys., 24,1905-1917, 2006)whichuseacombinationofEISCAT electrontemperaturemeasurementsfromthemainlandandSvalbardtotrackthemotionoftheOCFLB.WedemonstratewhetherusingtheInternationalReferenceIonospheremodel(IRI2007)canenhancethismethodandmakeitapplicabletootherincoherentscatterradars. InparticularwemakeuseofEISCAT datatoinvestigatetheelectrontemperaturesignaturesoftheOCFLB duringalargenumberofsubstorms.

P19ImagingobservationsofX-rayalbedoina

compactdiskflareMarinaBattaglia (UniversityofGlasgow)with

Eduard Kontar, and Iain Hannah

X-raysfromsolarflaresourcesareanimportantdiagnostictoolforparticleaccelerationandtransportinthesolaratmosphere. However, theobservedfluxatEarthiscomposedofdirect

emissionandphotonswhichareComptonbackscatteredfromthephotosphere. Thiscontributioncanaccountforupto40%oftheobservedfluxatenergiesof30-50keV,evenforanisotropicsource. Wepresentimagingobservationsofacompactflareonthesolardisc.Thesourcefull-width-halfmaximumwasdeterminedatdifferentenergiesusingX-rayvisibilityforwardfitting. Theobservedsourcesizeincreasesanddecreaseswithenergywithamaximumsizeatabout40keV,contrarytoobservationsmadeinlimbevents. ThebehaviourisconsistentwithpredictionsfromMonteCarlosimulationsofX-rayphotontransportinwhichX-rayvisibilitieswerecomputedfromsimulatedmapsandfittedusingvisibilityforwardfit.

ParallelelectricfieldgenerationbyAlfvénwaveturbulence

NicolasBian (UniversityofGlasgow)withEduard Kontar, and John Brown

WeinvestigatethespectralstructureoftheparallelelectricfieldgeneratedbystronganisotropicAlfvénicturbulence, inrelationwiththeproblemofaccelerationandheatinginastrophysicalplasmas, includingflareselectrons. A low-β two-fluidMHD modelisusedtofollowtheturbulentcascaderesultingfromthenon-linearinteractionbetweenkineticAlfvénwaves, fromthelargeMHD scalesdowntothesmall"kinetic"scales.ScalingrelationsareobtainedforthemagnitudeoftheelectromagneticfluctuationsshowingtheturbulentelectricfielddevelopsacomponentparalleltothemagneticfieldatlargeMHD scales.Thespectrumoftheparallelelectricfieldcanbeeffectivelyusedtomodelstochasticaccelerationofelectronsduringsolarflares. Thequasi-linearmodelingoftheaccelerationprocessisdiscussed.

ParticleaccelerationattheSunPhilippaBrowning (JBCA,Universityof

Manchester)

Thisinvitedtalkwillgiveanoverviewofparticleaccelerationinsolarflares. Observationalaspectsofhighenergyparticlesinflareswillbebrieflysummarised. Themaintheoreticalmodelsofaccelerationonflareswillbeoutlined, focusingonmodelsofparticleaccelerationinreconnectingmagneticfields. Somechallengesforfutureworkwillbeproposed.

ParticleAccelerationinthePresenceofWeakTurbulenceatanX-TypeNeutralPoint

ChristinaBurge (UniversityofGlasgow)withAlec MacKinnon, and Panagiota Petkaki

Itiswellknownthatparticlesinspaceplasmascanbeenergisedbyinteractionwithreconnectionregions, whichformatmagnetictopologicalfeaturessuchasnullsandseparatrices.Suchenergisationhasbeenstudiedinsimple, large-scalefields. Hereweextendthesestudiestoincludenoisy, turbulentelectricandmagneticfields.Themagneticfieldisperturbedbyasuperpositionofcoldplasmaeigenmodes,includingself-consistentelectricfieldoscillations,constructedasintheworkofCraigandMcClymont. Weakturbulenceismodelledbyadoptingrandomphasesfortheseeigenmodes.Usinganadaptivestepsizemethodwenumericallyintegrateparticleorbitsinrealisationsofthisfieldanddescribetheresultingparticledistributions.

Roleoflatitudeofsourceregioninsolarenergeticparticleevents

SilviaDalla (JeremiahHorrocksInstitute, UCLan)with Neus Agueda(UC Berkeley)

MeasurementsofSolarEnergeticParticles(SEPs)ininterplanetaryspacecanbeusedtoconstrainmodelsoftheiraccelerationduringeruptiveeventsattheSun, providedthattherolesofmagneticconnectiontothesourceandofinterplanetarytransportareunderstood. ItiswellknownthatthelongitudeofthesourceregionattheSunisakeyparameterindeterminingwhetheranSEP eventwillbedetectedanditscharacteristics.

HerewediscusshowthelatitudinalseparationbetweensourceregionanddetectingspacecraftinfluencestheprobabilityofobservingSEPsat1AU.Weselectasampleof477solarflaresofmagnitudegreaterthanC8.0, locatedinthewell-connectedlongitudinalrangebetweenW20andW80, andanalysewhetherornotanassociatedSEP eventisdetectednear-Earth. WeconsiderprotonmeasurementsbyGOES andelectrononesbyWIND/3DP.

Theseparationinheliolatitudebetweeneachflareregionanddetectingspacecraft, D,variesbetween0and30degreesinthissample. WefindanincreasedprobabilityofSEP detectionforDbetween4and12degrees. ValuesofD below4degreesandbetween12and28degreesarecharacterisedbyanSEP probabilityabouthalfthatinthe4-12degreerange.

MeasurementofAnisotropyinSolarFlareElectronSpectrausingRHESSI HardX-Ray

Spectroscopy.EwanDickson (UniversityofGlasgow)with

Eduard Kontar

Theangulardistributionofelectronsacceleratedinsolarflaresisakeyparameterinunderstandingtheaccelerationandpropagationmechanismsthatoccurthere. Howeverthisanisotropyisstillapoorlyknownquantitywithobservationalstudiesproducingevidenceforanisotropicdistributionandtheoreticalmodelsmainlyconsideringthestronglybeamedcase. Theeffectofphotosphericalbedocanbeusedtoinferthisanisotropyasitinfluencesdifferentlydirectedphotonsallowingdiagnosticsoftheangulardistributionintheelectrondistribution. A bi-directionalapproximationwasappliedandaregularizedinversionwasperformedonHardX-rayobservationsmadebyRHESSI inordertodeducetheelectronspectrainbothdownward(towardsthephotosphere)andupward(awayformthephotosphere)directions. Todetermineiftheanisotropychangessignificantlyovershortperiodsoftime. Intervalslasting4, 8and16seconds, overtheimpulsivepeakoftheflarewereexaminedforanychangeinanisotropy. ThiswasappliedtofoursuitableflaresdetectedbyRHESSI.Thedistributionsdeterminedwereconsistentwiththeisotropiccase.

Particleaccelerationinafragmentingcurrentsheet

MykolaGordovskyy (UniversityofManchester)with P.K. Browning, and G.E. Vekstein

Protonandelectronaccelerationisinvestigatedbasedontheforcedreconnectionmodelinwhichtheinitialcurrentsheetfragmentsintoaseriesoflocalisedcurrentfilamentsandmagneticislands.WeusecombinationofMHD andtest-particleapproachestoconsiderparticletrajectoriesconsistentlywithatime-dependentreconnection

68 P18–P19

model. Itisshownthatacceleratedparticlesinsuchamodelformtwodistinctivepopulations.ProtonsandelectronsmovinginopenmagneticfieldhaveenergyspectrawhichareacombinationoftheinitialMaxwelliandistributionandapower-lawhigh-energy(> 10keV) tail. Thesecondpopulationcontainsparticlesmovinginclosedmagneticfieldaroundo-points. Theseparticlesmovepredominantlyalongtheguidingfieldandtheirenergiesfallwithinquiteanarrowrangebetween100keV and10MeV.Itwasalsofoundthatparticlesmovinginclosedmagneticfieldhaveconsiderablyhigherpitch-anglesthanthosemovingintheopenconfiguration.

ParticleMotionandEnergyGainsinKinematicMHD modelsofCollapsingMagneticTrapsKeithGrady (UniversityofStAndrews)with

Keith Grady, and Thomas Neukirch

Duringsolarflaresalargenumberofchargedparticlesareacceleratedtohighenergies, buttheexactmechanismresponsibleforthisisstillunclear. Accelerationincollapsingmagnetictrapsisoneofthemechanismsproposed. WediscussanalyticidealkinematicMHD modelsforcollapsingmagnetictraps. Particleorbitsarecalculatedusingtheguidingcentreapproximation. Anillustrativeexampleofacollapsingmagnetictrapmodelwillbepresentedtogetherwithsomestudiesoftheeffectsoftheinitialconditionsoftheparticlesonthetrappingtimesandparticleenergygains.

Temporal, Spectral, andSpatialAnalysesofX-rayEmissionComponentsinImpulsiveSolarFlares

JingnanGuo (UniversityofGlasgow)withSiming Liu, Lyndsay Fletcher, and Eduard Kontar

Plasmaheatingandparticleaccelerationarethekeyissuesinsolarflarestudy. TwodistinctX-rayemissioncomponentsareoftenidentifiedinsolarflare. Theimpulsive, non-thermalhardX-raycomponentnormallyoriginatesfromthechromosphericfootpoints, whilethemoregradualthermalandsoftX-rayemissionoftenoriginatesfromcoronalsources. UsingRHESSI X-raydatawecalculatethetime-derivativeofsolarflarephotonlightcurvesindifferentenergybands. Theenergydependenceofthefluxchangerateanditstimeevolutionisstudiedforawellobservedsolarflare.A lower(higher)rateisexpectedforthelower(higher)energycomponent, andthetransitionenergybetweenthelowandhighratecomponentswillbecomparedwiththetransitionenergybetweenthethermalandnonthermalcomponents.Thisstudywillhelpusquantitativelyunderstandtherelationbetweenenergeticnon-thermalelectronsandhotplasmasresponsiblefortheobservedsoftX-rays. ThisworkissupportedbytheEU'sSOLAIRE ResearchandTrainingNetworkattheUniversityofGlasgow(MTRN-CT-2006-035484).

Cantheinfluenceofturbulentdensityperturbationsinthecoronabedetectedinflare

X-rayspectrum?IainHannah (UniversityofGlasgow)with

E.P. Kontar, and H.A.S. Reid

RHESSI solarflarehardX-rayobservationssometimescannotbeadequatelyinterpretedintermsofpurelycollisionalelectrontransport. Weinsteadpresentnumericalsimulationswhereweconsidertheenergeticelectron-beaminteractionsinthepresenceoflowfrequencydensityperturbations. Wedemonstratehowtheturbulentdensityperturbationsaffectthehighfrequency

Langmuirwavesandinturn, theflareacceleratedelectrondistribution. Theconsequencesofthisself-consistenttreatmentarediscussedfortheobservableX-rayspectrum.

CoronalmagnetictopologyandthesolarsourceofmajorSEP events

ChuanLi (UniversityCollegeLondon–MSSL) withC.J. Owen, S.A. Matthews, Y. Dai, and Y.H. Tang

A statisticalsurveyofthemajorelectroneventsduringtheperiod2002Februarythroughtheendofsolarcycle23ispresented. Wehaveobtainedelectronreleasetimesandthepeakfluxspectra.Wealsoderivedthecoronalmagneticconfigurationsoftherelatedsolaractiveregions(ARs)fromthepotential-fieldsource-surface(PFSS)model. Itisfoundthat: (1)11ofthe12openmagneticfield-lineeventsareprompteventswhoseparticlereleasetimescoincidewiththemaximaofflareemission. 13ofthe14closedmagneticfield-lineeventsaredelayedones, theexceptionalprompteventisassociatedwithalarge-scalecoronaldisturbanceordimming. (2)Anaveragedharderspectrumisfoundinopenmagneticfield-lineeventscomparedwiththeclosedones. Additionally, anobvioushigherrolloverenergyisseeninclosedmagneticfield-lineeventscomparedwiththeopenones. Thesecorrelationsclearlyestablishasignificantlinkbetweenthecoronalmagneticfield-linetopologyandtheescapeofchargedparticlesfromthesolarAR intointerplanetaryspaceduringthemajorsolarenergeticparticle(SEP) events.

StochasticParticleAccelerationbyCompressiveModeswithIncompressiveModeInducedSpatial

DiffusionSimingLiu (UniversityofGlasgow)with

Lyndsay Fletcher, and Eduard Kontar

Theinteractionbetweenlarge-scaleplasmafluctuationsandenergeticparticlesisoftenbelievedtobetheprocessresponsibleforparticleaccelerationinvariousastrophysicalsituations.Non-resonantstochasticinteractionsofparticleswithlarge-scalecompressivewavemodesleadtosecond-orderFermiacceleration. Thedetailsofthisaccelerationdependnotonlyonthespectrumofthecompressivemodesbutalsoontheparticlespatialdiffusioncoefficient. Sinceincompressivemodesaremoreefficientthancompressivemodesinscatteringoftheparticlesforthecompressivewavespeedhigherthantheincompressiveeddyspeed, boththecompressibleandincompressiblemodesplaycrucialrolesindeterminingtheresultantparticledistribution. Wewillreportouron-goinginvestigationofstochasticparticleaccelerationbyaspectrumofcompressiveandincompressivemodes. ThisworkissupportedbytheEU'sSOLAIRE ResearchandTrainingNetworkattheUniversityofGlasgow(MTRN-CT-2006-035484).

FromelectronmapstoaccelerationmechanismsofenergeticparticlesintheflaringSun

MichelePiana (Universita'diGenova)withA. GordonEmslie(OklahomaStateUniversity),

and Massone(CNR - SPIN),and Anna Maria(CNR- SPIN)

Imagingspectroscopyinvolvesinversionofbothspatialandspectraldatatoyield‘insitu’informationonthesourceasafunctionofbothenergyandposition. Inthespecialcasewherethespatialinformationisencodedintheformofvisibilities(two-dimensionalspatialFouriertransformsofthesourcestructure)itis

advantageous, bothconceptuallyandcomputationally, toperformfirstthespectralinversion, whichyieldsvisibilitiesoftheunknownsourcefunction; andthentospatiallytransformthesesourcefunctionvisibilities, whichyieldsmapsofthesourcefunctionatdifferentenergies.ForthevisibilitiesobservedbytheReuvenRamatyHighEnergySolarSpectroscopicImager(RHESSI)thisapproachhasbeenappliedforimagingspectroscopyanalysisofhardX-rayemissionduringsolarflares. Thisprocedureinvolves:regularizedinversionofthecountvisibilityspectratoobtainsmoothedformsofthecorrespondingelectronvisibilityspectra; applicationofconventionalvisibility-basedimagingalgorithmsthatyieldsimagesoftheelectronfluxthatvarysmoothlywithenergy.

ThepresenttalkwillshowhowsuchanapproachcanbeutilizedtoinferquantitativeinformationontheaccelerationmechanismsoccuringinsolarplasmaduringtwoflaringeventsobservedbyRHESSI.Morespecifically, inthecaseofthesolarflareobservedonFebruary202002, wewillshowthatRHESSI dataareconsistentwithCoulombcollisionsbetweenanaccelerationsitehighinthecoronaandthedensechromosphericfootpointregions; andthatananalysisofthecentroidpositionsoftheseelectronmapsallowsustoinferthedensitystructureinthetwovisiblecompactsources. Then, fortheNovember032003solarflare, wewillshowhowPetrosianandChen(2010)couldusethismethodandthehigh-resolutionX-rayobservationsprovidedbyRHESSItoderiveseveralimportantparametersofthestochasticmodelforparticleacceleration.

Electromagneticemissionfrombeam-generatedLangmuirwaves

HeatherRatcliffe (UniversityofGlasgow)

Thebeamsofflare-acceleratedelectronsinthesolarcoronahavebeenextensivelystudiedandareknowntoproducehighlevelsofLangmuirwaves.Thesemayinturnproduceelectromagneticemission, boththroughscatteringbythermalionsintheplasma, orbya3-wavedecayprocessinvolvingion-soundwaves. Bothoftheseproduceradiationneartheplasmafrequency, andarepossiblemechanismsforTypeIII radioemissionneartheplasmafrequency. Becausethelatterrequiresappreciablelevelsofionsoundwavestobepresentitisonlyofinterestwheretheelectrontemperaturefarexceedstheiontemperature; theformermayoccurwhentheiontemperatureissimilar, orgreaterthan, theelectrontemperature.Thesituationmaybetreated1-dimensionally, byassumingthetransversewavesareemittedperpendiculartotheLangmuirwaves. Thekineticequationscanthenbesolvednumerically, usingafirstorderfinitedifferenceintegrationscheme; thisisdoneforahomogeneousplasmaatadensitytypicalofthesolarcorona.Someresultsforthespectrumofplasmaemissionarepresentedforvaryingvaluesoftheelectronandiontemperatures, anddifferentfunctionalformsfortheinitialLangmuirwavespectrum.

SolarFlareAcceleratedElectronTransportthroughtheTurbulentDensityoftheSolarWind

HamishReid (UniversityofGlasgow)withEduard Kontar

SolarflareacceleratedelectronbeamspropagatingawayfromtheSuncaninteractwiththeturbulentinterplanetarymedia, producingplasmawavesandtypeIII radioemission. TheseelectronbeamsaredetectedneartheEarthwithadoublepower-

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lawenergyspectra. WesimulateelectronbeampropagationfromtheSuntotheEarthintheweakturbulentregimetakingintoaccounttheself-consistentgenerationofplasmawavesandsubsequentwaveinteractionwithdensityfluctuationsfromlowfrequencyMHD turbulence.Therateatwhichplasmawavesareinducedbyanunstableelectronbeamisreducedbybackgrounddensityfluctuations, mostacutelywhenfluctuationshavelargeamplitudesorsmallwavelengths. Thissuppressionofplasmawavesaltersthewavedistrubtionwhichchangestheelectronbeamtransport. Assuminga5/3Kolmogorov-typepowerdensityspectraoffluctuationsoftenobservedneartheEarth, weinvestigatethecorrespondingenergyspectraoftheelectronbeamafterithaspropagated1AU.Wefindadirectcorrelationbetweenthespectraofthedoublepower-lawbelowthebreakenergyandtheturbulentintensityofthebackgroundplasma. Foraninitialspectralindexof3.5, wefindarangeofspectrabelowthebreakenergybetween1.7-2.1,withhigherlevelsofturbulencecorrespondingtohigherspectralindices.

Numericalsimulationofmagnetosphericelectroncyclotronemission

DavidSpeirs (DepartmentofPhysics, UniversityofStrathclyde)with K. Ronald, K.M. Gillespie,S.L. McConville, A.D.R. Phelps, A.W. Cross,

R. Bingham, B.J. Kellett, R.A. Cairns, and I. Vorgul

Whenaninitiallymainlyrectilinearelectronbeamissubjecttosignificantmagneticcompression,conservationofmagneticmomentresultsintheformationofahorseshoeshapedvelocitydistribution. Ithasbeenshownthatsuchadistributionisunstabletocyclotronemissionandmayberesponsibleforthegenerationofplanetaryandstellarauroralradioemissions. Principlecharacteristicsofsuchemissionsincludeahighdegreeofextraordinary(X) modepolarizationandaspectraloutputcomprisingwelldefinedcomponentsextendingdowntoalowerfrequencycut-offcorrespondingtothelocalrelativisticelectroncyclotronfrequency. PiC codesimulationshavebeenundertakentoinvestigatethedynamicsofthecyclotronemissionprocessintheabsenceofradiationboundarieswithparticularconsiderationofthespatialgrowthrate,spectraloutputandRF conversionefficiency.Computationsrevealthatawell-definedcyclotronemissionprocessoccursalbeitwithareducedspatialgrowthratecomparedtowaveguideboundedsimulations. RF outputisnearperpendiculartotheelectronbeamwithaslightbackward-wavecharacterthatisalsoreflectedinthespectraloutput. ThecorrespondingRFconversionefficiencyof1.1%iscomparabletowaveguideboundedsimulationsandconsistentwiththepredictionsofkinetictheorythatsuggestefficient, spectrallywelldefinedemissioncanbeobtainedfromanelectronhorseshoedistributionintheabsenceofradiationboundaries.

MagnetosphericParallelElectricFieldsCraigStark (UniversityofSt. Andrews)with

A.N. Wright, and A.P. Cran-McGreehin

Field-alignedcurrentsobservedalongtheEarth’smagneticfieldcoupletheionospheretothemagnetosphere. Suchcurrents, andtheirassociatedparallelelectricfields, areresponsiblefortheobservedauroraandplayasignificantroleintheglobalcurrentnetworksurroundingtheEarth. Byconsideringthemotionoftheiono-magnetosphericplasma, undertheinfluenceofabackgroundelectromagneticfield, onecanobtain

aquasi-steadystateelectricfielddistributionalongthemagneticfieldwhilepreservingquasi-neutrality. Theaimofthisresearchistounderstandhowtheimplicatedplasmasrespondtothesefields, howthisvarieswithspeciestemperature, theprescribedelectricfieldstrengthandaltitude. Wepresentaplasmakinetictreatment, analysinghowthevelocitydistributionfunctionsevolvealongamagneticfluxtube,takingintoaccountmirroringandprecipitatingpopulations. Bycalculatingthemomentsoftheresultingdistributionfunctionsweascertainhowthecollectiveelectromagneticandpressureeffectsactingontheplasmaarebalancedandmaintained, establishingadynamicequilibrium.Herewediscussourkineticplasmamodelandpresentwork-in-progress, preliminaryresults.

Electronsre-accelerationatthechromosphericfootpointsofSolarFlares

RimTurkmani (ImperialCollege)with John Brown,Eduard Kontar, Alec MacKinnon, and

Loukas Vlahos

Traditionallyacceleratedelectronsinsolarflaresarethoughttobeacceleratedinthecoronalpartoftheloop, andthentraveltothefootpointswheretheylosetheirenergyandradiatetheobservedHardX-ray. Werevisitthisassumptionbackedwithincreasingobservationalevidencethatchallengesthissimplifiedpicture. WeproposeanewLocalRe-accelerationThickTargetModel(LRTTM) whereatthefootpointselectronsreceiveaboostofre-accelerationinadditiontotheusualcollisionalloses. Suchmodelmayofferanalternativetothe‘standard’collisionalthicktargetinjectionmodel(TTM) (Brown1971)ofsolarHXRburstsources, requiringfarfewerelectronsandsolvingsomerecentproblemswiththeTTMinterpretation. Welookatthedifferentscenariosthatcouldleadtosuchre-accelerationandpresentnumericalresultsfromoneofthem.

AuroralParticleAccelerationattheEarthAndrewWright (UniversityofStAndrews)

Anoverviewisgivenoftheoriginofparticleaccelerationintheterrestrialauroralcurrentsystem. Theseparticlesareimportantincouplingthemagnetospheretotheionosphereviaelectricalcurrentsthatflowalongmagneticfluxtubes, andarealsoresponsibleforproducingthevisibleaurora. Examplesofspacecraftparticledatawillbeusedtoillustratesomeofthemainaccelerationmechanisms.

P20TheGRB-SN connection: ExploringGRB

progenitorswithmulti-wavelengthobservationsZachCano (ARI,JohnMooresUniversity

Liverpool)

OveradecadeagotheGRB-SN connectionwashintedat, andlaterconfirmedspectroscopicallyin2003. Duringthisperiodithasbeenshownthatatleastsome, ifnotalllong-durationGRBsarecausedbythecore-collapseofamassivestarintoatypeIcSN.AlthoughanabsoluteconnectionofaGRB toaSN canonlybedonespectroscopically,photometricevidenceofSN "bumps"inGRB LCsthatareaccompaniedbyachangeincolourprovidecircumstantialevidenceforaconnectionbetweenGRBsandthecollapseofmassivestars.

Usingdatatakenonnumeroustelescopes,includingseveralepochsonHST,threelinesofevidenceareprovidedforaconnectionofaredSN withGRB 060729. SN "bumps"areseeninthelight-curvesthatareaccompaniedbyachangeincolour, andatlatetimesthespectrumoftheOTresemblesthatofthearchetype1998bw, onlyredder.

FurtherevidenceisalsogivenforanassociationofaSN withGRB 090618. A beautifully-detailedandwell-sampledlight-curvehasbeenobtained,andredSN "bumps"areseen. ThoughbothoftheGRBsarelocatedatthesamecosmologicaldistance(z=0.54), theSNeappeardifferent. TheseresultsfurthervindicatetheGRB-SN connection,concludingthatwhileaGRB islikelyformedduringthecollapseofamasivestar, theresultingSNearesubstantiallydifferent.

GRB090510, thefirstcasestudyofashortGRBwithGeV extendedemissiondetectedbyFermi

andSwift.MassimilianoDePasquale (UniversityCollege

London–MSSL) with SwiftTeam, FermiGBMCollaboration, and LAT Collaboration

Thebright Γ−RayBurstGRB 090510wasunprecedentedasthefirstshortGRB detectedsimultaneouslybySwift-XRT &UVOT andFermi-LAT,coveringtheenergyrangefrom0.002keV tomorethan300GeV.ExtendedGeV emissionwasdetectedbyFermi-LAT,lastingfor200saftertheinitialtrigger, andityieldedthehighestenergyphotoneverobservedfromashortGRB (30.5GeV).Wereportonthejointmulti-wavelengthobservationsofGRB 090510performedbyFermiandSwift. ThisexceptionalGRB enabledustoinvestigatethephysicalpropertiesoftheGRBoutflow, poorlyunderstoodinshortbursts. Wediscussinternalandexternalshockmodelsforthebroadbandenergyemissionofthisobject.

Identifyingandchacterisingtheprogenitorsofcore-collapsesupernovae

MorganFraser (QueensUniversityBelfast)withA. Pastorello, S. Smartt, and K. Takats

Core-collapsesupernovae(SNe)arethespectacularend-pointsofstellarevolution. Notonlyaretheyakeytestforstellarevolutionarymodels, buttheyarealsoanopportunitytostudythephysicsunderlyingsomeofthemostenergeticeventsintheUniverse. DetectingtheprogenitorsoftheseSNeinarchivalimagesallowsustodirectlylinkmassivestarstosupernovae, andindoingso, tounderstandhowthepropertiesoftheprogenitor(mass, metallicityetc.) affectthecharacteristicsandevolutionofthesupernova, andultimatelyleadtothedifferentsupernovasubtypes.

Wepresentrecentresultsfromoursupernovaprogenitorprogram, focusinginparticularontheTypeII SN 2009kr, whereweidentifyacandidateprogenitorinarchivaldatafromtheHubbleSpaceTelescope. Thecandidatewefind, ifasinglestar,isconsistentwithayellowsupergiantprogenitor,whichisincontrasttotheredsupergiantprogenitorfoundforallotherTypeIIP SNesofar.

HighlightsfromFermiobservationsofGamma-RayBursts

JonathanGranot (UniversityofHertfordshire)

TheFermi Γ−RaySpaceTelescopehasmorethandoubledthenumberof Γ−RayBursts(GRBs)detectedathighenergies(> 100 MeV) withinitsfirstyearofoperation. Thankstotheverywide

70 P19–P20

energyrangecoveredbyFermi's Γ−rayBurstMonitor(GBM;8keV to40MeV) andLargeAreaTelescope(LAT;25MeV to > 300 GeV) ithasmeasuredthepromptGRB emissionspectrumoveranunprecedentedlylargeenergyrange(from∼ 8 keV to ∼ 30 GeV).I willpresenthighlightsofFermiGRB observationsoveritsfirst1.5yearsofoperation, focusingmainlyonthepromptemissionphase. Interestingnewobservationswillbediscussedalongwithsomeoftheirpossibleimplications, including:

(i)WhatcanwelearnfromtheFermi-LAT GRBdetectionrate,

(ii)A limitonthevariationofthespeedoflightwithphotonenergy(forthefirsttimebeyondthePlanckscaleforalinearenergydependencefromdirecttimeofarrivalmeasurements),

(iii)Lower-limitsonthebulkLorentzfactoroftheGRB outflow(of ∼ 1000 forthebrightestFermiLAT GRBs),

(iv)Thedetection(orinothercases, lackthereof)ofadistinctspectralcomponentathigh(andsometimesalsoatlow)energies, andpossibleimplicationsforthepromptGRB emissionmechanism,

(v)Thelateronset(andlongerduration)ofthehigh-energyemission(> 100 MeV) comparedtothelow-energy(< 1 MeV) emissionthatisseeninmostFermi-LAT GRBs.

Discoveryofanunusualnewradiosourceinthestar-forminggalaxyM82: Faintsupernova,

supermassiveblackhole, oranextra-galacticmicroquasar?

TomMuxlow (JodrellBankCentreforAstrophysics)with Rob Beswick, Simon Garrington, Alan Pedlar,

Danielle Fenech, Megan Argo,Janinevan Eymeren, Martin Ward, Andreas Zezas,

and Andreas Brunthaler

A faintnewradiosourcehasbeendetectedinthenuclearregionofthestarburstgalaxyM82usingMERLIN radioobservationsdesignedtomonitorthefluxdensityevolutionoftherecentbrightsupernovaSN2008iz. Thisnewsourcewasinitiallyidentifiedinobservationsmadebetween1-5thMay2009buthadnotbeenpresentinobservationsmadeoneweekearlier, orinanypreviousobservationsofM82. Inthispaperwereportthediscoveryofthisnewsourceandmonitoringofitsevolutionoveritsfirst9monthsofexistence. Thetruenatureofthisnewsourceremainsunclear, andwediscusswhetherthissourcemaybeanunusualandfaintsupernova, asupermassiveblackholeassociatedwiththenucleusofM82, orintriguinglythefirstdetectionofradioemissionfromanextragalacticmicroquasar.

Searchforgravitational-waveinspiralsignalsassociatedwithshortGamma-RayBurstsduring

LIGO'sfifthandVirgo'sfirstsciencerunValeriuPredoi (CardiffUniversity)with LIGO

ScientificCollaboration, and VirgoCollaboration

Oneofthemostcommonlyacceptedcandidatesourcesforshorthard γraybursts(SHB) isthemergerofcompactbinaryobjects, i.e. eitherneutronstar-neutronstarorneutronstar-blackholebinarysystems. Suchmergersarealsopredictedtoemitstronggravitationalradiationwithwaveformsthatcanbedescribedtheoretically. Wepresentasearchfortheseknowngravitational-wavesignaturesintemporalanddirectionalcoincidencewith22SHBsdetectedby γraytelescopesduring

LIGO'sfifthsciencerun, S5, andVirgo'sfirstsciencerun, VSR1. Thedatareductionpipelinemakesuseofmatchedfilteringofthegravitationalwavedetectoroutputagainstatheoreticalwaveformtemplatebank. Wefindnostatisticallysignificantgravitational-wavecandidateswithina[-5, +1)swindowaroundthetimeofanyGRB.Usinganadequatestatisticaltest, wefindnoevidenceforanexcessofweakgravitational-wavesignalsinoursampleofGRBs. Weexcludeneutronstar-blackholeprogenitorstoamedian90%CL exclusiondistanceof6.7Mpc.

DiscoveryoftheafterglowandhostgalaxyofthelowredshiftshortGRB 080905A

AntoniaRowlinson (UniversityofLeicester)withK. Wiersema, A.J. Levan, N.R. Tanvir, P.T. O'Brien,

andothers

WepresentthediscoveryofshortGRB 080905A,itsopticalafterglowandhostgalaxy. InitiallydiscoveredbySwift, ourdeepopticalobservationsenabledtheidentificationofafaintopticalafterglow, andsubsequentlyaface-onspiralhostgalaxyunderlyingtheGRB position. Furthermorethereisnosupernovacomponentpresentintheafterglowtodeeplimits. Spectroscopyofthegalaxyprovidesaredshiftofz=0.1218, thelowestredshiftyetobservedforashortGRB.TheGRB liesoffsetfromthehostgalaxycentreby ∼ 18.5 kpc,inthenorthernspiralarmwhichexhibitsanolderstellarpopulationthanthesouthernarm. Noemissionlinesarevisibledirectlyundertheburstposition, implyinglittleongoingstarformationattheburstlocation. ThesepropertieswouldnaturallybeexplainedweretheprogenitorofGRB080905A acompactbinarymerger.

LuminoustransientsinthedistantuniversewithPTF andSNLS

MarkSullivan (UniversityofOxford)

TheSupernovaLegacySurvey(SNLS) andthePalomarTransientFactory(PTF) arebothrollingtransientsurveys, designedtosurveydistantcosmicexplosionswithoutregardtohostgalaxytypeorenvironment, andarethusfreefromthebiasesassociatedwithearliergalaxy-targetedprogrammes. Bothsurveysareuncoveringnewtypesandexamplesofsupernovaexplosionswithunprecedentedultra-violetluminosities, locatedatsomeofthehighestredshiftsyetdiscovered. Inthistalk, I willpresentthelatestresultsonthistopicfrombothsurveys.

InvestigationoftheenvironmentofshortgammarayburstGRB090510withaviewtoconstraining

theprojenitor.RachelTunnicliffe (UniversityofWarwick)with

A. Levan

Investigationoftheenvironmentsoflong ΓRayBursts(GRBs)hasshownthemtobeassociatedwithmassivestarsandhencehasgonesomewaytoidentifyingtheirprojenitors. A similarprocedureisrequiredforshort, hardburstsofwhichtherearefewerwellobservedeventsmeaningafullinvestigationofeveryburstisimportant. WehaveanalysedtheburstandenvironmentofGRB 090510, basedonNOT andVLT observations. ThisburstwasalsospectacularlydetectedbyFermiouttoenergiesinexcessof30GeV.Becauseofthis, italsoprovidesunprecedentedinsightintopossibleLorentzInvarianceViolations, althoughthisdependscruciallyontheknownburstredshift. Usingtheopticalafterglowwepinpointthelocationofthebursttooccurringsome7kpcfromthecoreofa

quiescentgalaxyatz=0.903. Thecharacteristicsofthishost, andtheoffsetoftheburstfromit, areinconsistentwiththepropertiesoflongGRBs, butbroadlyconsistentwiththoseofthesmallsampleofshortGRB hosts. ThisisinkeepingwiththeexpectationsofmodelsfortheproductionofshortGRBsincompactbinarymergers.

P21TeVeS andthestraightarcofA2390

MartinFeix (UniversityofStAndrews)withHongsheng Zhao, Cosimo Fedeli,

JoséLuisGarrido Pestaña, and Henk Hoekstra

Wesuggesttotestthecombinedframeworkoftensor-vector-scalartheory(TeVeS) andmassiveneutrinosingalaxyclustersviagravitationallensing, choosingthesystemA2390withitsnotoriousstraightarcasanexample. Adoptingquasi-equilibriummodelsforthemattercontentofA2390, weshowthatsuchconfigurationscannotproducetheobservedimage. Generally, nonlineareffectsinducedbytheTeVeS scalarfieldareverysmall, meaningthatcurleffectsarebasicallynegligible. Basedonthisresult, weoutlineasystematicapproachonhowtomodelstronglensesinTeVeS,whichisdemonstratedforA2390.Comparedtogeneralrelativity, weconcludethatdiscrepanciesbetweentheindependentmassestimatesfromlensingandX-rayobservationsareamplified. Finally, weaddressthequestionofthemodel’sfeasibilityandpossibleimplications/problemsforTeVeS.

Thenewpathtotimedelays?GülayGürkan (TheUniverstiyofManchester)with

Neal Jackson

Tobetterunderstandtheuniverseanditsdynamics, theHubbleconstantisacrucialparameterwhichprovidesvaluableinformationabouttheexpansionrateoftheuniverse. Sofar,theHubbleconstanthasbeendeterminedbyvariousmethodssuchasCepheidvariablesbyutilizingHST KeyProjectdataandWMAP.TheaccuracyoftheHubbleconstantvalueisnotbetterthan10%duetointrinsicconstraints/assumptionsofeachmethod.

GravitationallenssystemsprovideanotherprobeoftheHubbleconstantusingtimedelaymeasurements. CurrentinvestigationsoftimedelaylenseshaveresultedindifferentvaluesofHorangingfrom50-80km/s/Mpc. Themainproblemingravitationallenssystemsisthatrequiresamassmodelforthelenswhichisdifficulttomeasureindependentlyunlessobservationalconstraintsareavailable. Moreover, inordertoseetimedelaysclearly, fluxesofsourceshavetobevariable. Ontheotherhand, usingatypicalvalueoftheHubbleconstantandmeasuredtimedelaysenableustodetermineabetter/moreaccuratemassmodelforthelensgalaxy.

Hereweattempttodevelopanewandmoreefficientmethodformeasuringtimedelays, whichdoesnotrequireregularmonitoringwithahigh-resolutioninterferometerarrayorwithopticaltelescopes. Instead, theWSRT isusedforfluxmonitoringofdoubleimagelenssystemsinwhichthebrighterimageisexpectedtovaryfirst.TriggeredVLA observationscanthenbeusedtocatchthesubsequentvariabilityofthefainterimage. Wepresentpreliminaryresultsfromsuchaprogram.

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ProbingtheDarkUniversewithWeakLensingTomographyandtheCFHTLS

CatherineHeymans (IfA,UniversityofEdinburgh)with Emma Grocutt, Alan Heavens, Tom Kitching,

and CFHTLenS team

Weakgravitationallensingisapowerfultechniqueformeasuringthepropertiesofdarkmatteranddarkenergyfromtheirgravitationaleffectsalone.TheCanada-France-HawaiiTelescopeLegacySurveyiscurrentlythelargestdeepopticaldatasetforweaklensinganalysiscovering172squaredegreesover5opticalbands. Wepresentaninvestigationintotheoptimaltomographicthree-dimensionalanalysisoftheCFHTLS weaklensingsignalthatminimisestheimpactofsystematicsarisingfromintrinsicgalaxyalignments. Withsystematicsundercontrol, sincetheinfluenceofdarkenergyonstructuregrowthisredshift-dependent, tomographicanalysisofredshiftbinswillallowustoconstrainthepropertiesoftheDarkUniverse.

ApplicationsofaNewandRapidSimulationsMethodforWeakLensingAnalysis

AlinaKiessling (UniversityofEdinburgh)withAndy Taylor, and Alan Heavens

Gravitationallensingissensitivetoallgravitatingmass- bothBaryonicandDarkMatter- makingittheidealtooltostudyCosmologyindependentlyofanyassumptionsaboutthedynamicalorthermalstateofobjects. TheNextGenerationofSurveyTelescopewillobservemoreoftheskythaneverbeforeandthevolumeofdatatheywillproduceisunprecedented. Torealisethepotentialofthesesurveys, experimentsrequirefulllargeend-to-endsimulationsoftheSurveystotestanalysismethodsandproviderealisticerrors. Wehavedevelopedanewline-of-sightintegrationapproachtosimulating3-D WeakGravitationalLensShearandConvergencefields. Theselightconesarefastertogeneratethantraditionalray-tracing, sowecanrunanensembleofsimulationsallowingustogeneratecovariancematriciesforcosmologicalparameterestimationandstatisticalanalysis. Thispresentationwillintroduceournewanalysismethodanddiscusssomeofitsmanyapplicationsinweaklensingexperiments.

UsingtheLHC toprobeDarkMatterinphysicsbeyondtheStandardModel

DavidMiller (UniversityofGlasgow)

Ourextremelysuccessfulmodelofparticlephysics, theStandardModel, hasaprofoundflaw:ithasnoviablecandidatefordarkmatter. Inordertoincorporatedarkmatterintoourpictureoftheuniverse, wemustgobeyondtheStandardModeltotheoriessuchassupersymmetryorextradimensions. Ourcurrentdataindicatesadarkmattercandidatewithanelectroweakscalemass,exactlytherangethatwillbeprobedbythenewLargeHadronCollider(LHC).InthistalkI willreviewmodelsbeyondtheStandardModelthatprovideaviabledarkmattercandidateanddiscussthepotentialfortheirdiscoveryattheLHC.

BrightIdeasandDarkThoughts: "UniversalBaryonicScale"at"MaximumHaloGravity"

HongshengZhao (U.ofStAndrews(SUPA)) withGianfranco Gentile, Benoit Famaey, Paolo Salucci,

Andrea Maccio, Baojiu Li, Henk Hoekstra, andMartin Feix

I willinterpretaverycuriousconspiracyofdark-brightmatteringalaxies(Gentileetal2009Nature), insensitivetothesizesandformation

historiesoftheobservedgalaxies: thebaryonsareconcentratedtoapproximatelythesamesurfacedensityattheverypositionwherethehaloofferslocallymaximumgravity. Whilenormalgravitationalandgasfeedbackprocessesmustalwaysoccur, itisdifficulttoforgeafeedbackhistory-independentuniversalscaleunlessthereissomehelpfrompossiblynewphysicsintheDark.A partialconfirmationisseeninsimulationsofN-bodywherethematteriscoupledtoacosmologicalscalarfield(Zhaoetal. 2009, ApJLetters).

P22ImagingwithMIRC attheCHARA interferometer

FabienBaron (UniversityofMichigan)withJohn Monnier, Stefan Kraus, and Xiao Che

WepresenttherecentresultsobtainedwiththeMichiganInfraRedCombiner(MIRC) operatingattheCHARA interferometeratMountWilson, CA.Bycombininglightfromuptofourtelescopessimultaneously, MIRC allowsfastandmodel-independentimagingofstellarsurfacesorstellarsytemsatresolutionsbelowonemilliarcsecond.AmongsttheimagedobjectsaretherapidrotatingstarsAltairandAlderamin, thefamousinteractingbinariesBetaLyraeandAlgol, andthepeculiareclipsingsystemEpsilonAurigae. FinallyimagingYoungStarObjectswillbeattemptedaspartofthenextMIRC campaign, exploitingthepowerofthenew6-telescopefringe-trackingcapabilities.

ThecomplexinnerdisksofHerbigAeBestarsMyriamBenisty (INAF - Arcetri)with A. Natta,

A. Isella, E. Tatulli, F. Ménard, J.P. Berger, F. Massi,and F. Malbet

Understandingthephysicalconditionsintheclosecircumstellarenvironmentsofyoungstarsisacrucialsteptocomprehendplanetformationandevolution. Inthistalk, I willdiscussnear-infraredspectro-interferometricobservationsofHerbigAeBestars, thatallowedustodirectlyprobethehotcircumstellargasanddust. Thestructureoftheirinnermostregionshasbeenwidelydebatedandinthepastdecade, thegeneralconsensushasbeenthattheobservednearinfraredexcessisduetodirectthermalemissionfromhotdustlocatedattheirsublimationradius, inapuffed-uprim. Inthistalk, I willfirstpresenttwocasesthatsuggestthatthisdescriptionismaybetoosimple. I willshowlong-baselinespectro-interferometricobservationsoftheHerbigAestarHD163296obtainedwiththeAMBER instrumentattheVLTI,resultinginthelargestUV coverageachievedonayoungstartoday. Modelfittingofphotometricandinterferometricobservationssuggeststhatadominantcontributiontothenear-infraredemissionarisesfromanopticallythinregionextendingfromabout0.10to0.45AU,distancefromthestaratwhichanopticallythickdustydiskstarts. I willdiscussthenatureofthisemissionandwillarguethatitcouldtracethepresenceofveryrefractorygrainsratherthangas. I willalsopresentthecaseofHD100546, anoldHerbigBestar,thoughttohaveatransitionaldiskwithagap.Radiativetransfermodellingofthephotometricandinterferometricobservationsconfirmedthepresenceofthegap, constrainedthetotalmassofdustlocatedinsideitsinneredge, andallowedageneralstructureforthisevolveddisktobederived. Althoughgenerallyneglected, thisstudy,inaddition, showsthatscatteredthermallightcan

havealargecontributiontothenear-infraredcontinuumemission.

ScienceProspectswiththeMagdalenaRidgeObservatoryInterferometer(MROI)

DavidBuscher (UniversityofCambridge)withChris Haniff, and John Young

TheMagdalenaRidgeObservatoryInterferometerisanoptical/infraredaperturesynthesisinterferometerdedicatedtoimagingfaintobjectsatresolutionsdownto300micro-arcseconds. Itisbeingbuiltatahigh-altitudesiteinNewMexicobyapartnershipbetweentheUniversityofCambridgeandNewMexicoTech. Wegiveanoverviewofthetypesofhigh-angular-resolutionsciencethatMROI istargeting, includingstellarastrophysics, YSO disksandplanetformation, andAGN astrophysics. Wepresentanupdateonprogressonconstructionandanear-termtimelinefortheinterferometer.

ImagingshockfrontsinMiravariablesJamesGordon (UniversityofCambridge)with

David Buscher, and John Young

WediscusstheuseofhighangularresolutionopticalinterferometryforimagingshockfrontspropagatingthoughtheatmosphereofMiravariables. HighresolutionspectroscopyhaspresentedstrongevidencefortheexistenceofasupersonicshockevidentinBalmeremissionlines. Aperturemaskingandluckyimagingintheemissionlineatdifferentpulsationphaseswillallowustoreconstructimagesoftheshockfront.UnderstandingthepropertiesoftheshockisessentialforatmosphericmodelsandthecalculationofmasslossrateswhichhavedifficultyinaccountingforshocksinMiravariables.

DustydiscsaroundevolvedstarsFoteini(Claire)Lykou (JodrellBankCentrefor

Astrophysics)with Albert Zijlstra, andOlivier Chesneau

Wepresentthediscoveryofdusty, edge-ondiscsaroundevolvedstarsatdifferentevolutionarystages. Menzel3, M2-9andSakurai’sObjectwereobservedwithMIDI ontheVeryLargeTelescopeInterferometer(VLTI) providingaresolutionof∼ 0.01 arcsecinthemid-infrared. Thefirsttwoobjectscontaindiskscomposedofsilicatedust,whilethelastcontainsadisc-likestructureofcarbonaceousmaterial. Thedustydiscsarealignedwiththeminoraxisofthebipolarnebulae(oradensityenhancementontheroundnebulaforthelastobject)andtheirinnerrimradiiarelessthan100AU.Characterisingthedustydiscsinthecoreofthesenebulaeandatdifferentevolutionarystages, providesinvaluableconstraintsontheprocessesthatleadtotheseimpressivenebulae.Thepropertiesofeachdischavebeenexploredwiththemeansofradiativetransfermodelling.

Opticalandnear-infraredinterferometryofstarsanddisks

ReneOudmaijer (UniversityofLeeds)

Theseareexcitingtimesforopticalandnear-infraredinterferometry. Itisonlyinthelastfewyearsthatspectrallyresolvedinterferometryatmilli-arcsecondscaleshasbecomepossibleonaregularbasis, andthefuturepromisesevenmore.InthistalkI willreviewthelatestinterferometricresultsonbothyoungandevolvedstars.

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InvestigatingtheinnerdisksofyoungstarsJennyPatience (UniversityofExeter)with A. Binks,

R. Rhodes, and R. Akeson

WiththeexceptionalangularresolutionoftheKeckinterferometer, wearestudyingtheinnerdisksofyoungstarsatdifferentevolutionarystagesatspatialscalesoflessthan1AU.Thevisibilitiesofseveraltargetsindicatetheinnerdiskshavebeenspatiallyresolved. Thesizesoftheinnerdisksareestimatedbasedonmodelfitsandarecomparedwiththeexpectedradiusofdustsublimation, consideringtheluminosityofeachobject. Theestimatedinnerdiskradiioftheyoungstarsarealsocomparedwiththedistributionofcloseorbitextrasolarplanetstoinvestigateimplicationsforplanetmigration.

Mappingstar-spotsontheRS CVnbinary ζ AndEttorePedretti (SUPA,UniversityofStAndrews)with John Monnier, AndrewCollier Cameron,

Jean-Francois Donati, and Pascal Petit

WeobservedthemagneticallyactiveRS CVnbinaryZetaAnd=HD 4502usinglong-baselineinterferometryinordertodeterminethepolarspotstructure, whichhasbeendetectedbyZeeman-DopplerspectroscopyinseveralRS CVnbinaries.ThestarisanellipsoidalK giantbinarywhichhasbeenrecentlyimagedusingtheZeeman-Dopplertechnique. ThestarwasobservedattheCHARAinterferometerinAugust2007and2008. Theobtainedimagesshowasurfacewithasymmetricfeaturesconsistentwithstarspots.

TheMagdalenaRidgeInterferometerFringeTracker

AlexRea (UniversityofCambridge)withC. Jurgenson, F. Santoro, T. McCracken,

A. Olivares, D. Buscher, M. Creech-Eakman,C. Haniff, J. Young, A. Shtromberg, K. McCord,

and F. Baron

TheMagdalenaRidgeObservatoryInterferometer(MROI),acollaborationbetweenNewMexicoTechandtheUniversityofCambridge, willperformhigh-resolutionimagingdowntoalimitingmagnitudeofH=14. WereportonthestatusoftheMROI fringetracker, whoseperformancewillbecriticaltoreachingthislimitingsensitivity. Designoftheinstrumentiscomplete, andthefringetrackerisnowunderconstructionatMRO.Itconsistsofadedicated,near-IR,fringe-trackingbeamcombinerandspectrographs. Theinstrumentwillphaseuptheinterferometerbystabilizingfringesontheshorter"nearestneighbor"baselinesofthe"Y"-geometryarray, allowingforincreasedintegrationtimesonthelongerbaselinesandthebuildupofsignal-to-noiseinthescienceinstrument. Thebeamcombinerhasbeendesignedtoacceptlightfromamaximumoftentelescopes(threeoneacharrayarm, oneatthe"Y"vertex), butcanoperatewithfewerwithouthavingtochangetheoveralllayout.Eachspectrographwillmultiplexuptofivebeamcombineroutputsontoasingledetector. A pairofidenticalspectrographsareusedtosimultaneouslysamplecomplementaryfringepatternsthatareπradiansoutofphasewitheachother, reducingthenumberofmodulatorstepsneededtomeasurethefringephase.

Dosingleoldstarsejectclumps?AnitaRichards (JBCA,UniversityofManchester)with Indra Bains, Phil Diamond, Malcolm Grey,

Graham Harper, Jeremy Lim, Dinhvan Trung, andJeremy Yates

Radiointerferometricimagingofatsub-AUresolutionshowsthatthewindsaroundevolvedstarsarecurdledintoclumps. Inthezonewheredustformationiswelladvanced(&5stellarradii),outtomanytensR*, thewatermasercloudsareover-denseand, ifextrapolatedbacktothestellarsurface, theirbirthsizeswouldhavebeenoforder0.1R*. Istheclumpingscalesetbystarspots,possiblyrelatedtoconvectioncells? Thisraisestheintriguingpossibilitythatthechemistryaswellasthedensitycouldbedifferentiatedintheclumps.Alternatively, ifthepulsation-poweredmass-lossprocessissmooth, cloudsmightbearesultofdustformation. Interferometryatwavelengthsfromcmtoopticalpenetratesdifferentdepthsinthestellarphotosphere. e-MERLIN,theEVLA andALMA willhavethesensitivityandtheimagingfidelitytoresolvethesuggestedlargeconvectioncellsinredsupergiantsandAGB starsouttoafewhundredpc(orfurtherforRSG).Byobservingatsuccessivelylowerfrequenciesatsuitabletimeintervals, wewilltestwhetherindependent(convective)orcorrelated(pulsation-driven)disturbancesdominate. Co-ordinatedVLBA ande-MERLINmaserobservationswillshowwhetherstarspotsdirectlyleadtoSiO maserclumpsandwhetherthesesurvivethedustformationprocess. WehopethatthiswillcomplementedbyVLTI,MROI orotheroptical/IR interferometrywhichwouldrevealtherelativedistributionofhotandalsoofabsorbingmaterialinthestronglyconvectivezone. Moreover, existingobservationsshowthatthestarsareasymmetric. Persistentaxisymmetrywouldsuggestthatanorderedmagneticfieldisimportant(intheabsenceofdetectablerotationforeffectivelysolitarystars)whilstvaryingdirectionswouldsuggestcomplexpulsationmodes.

ResolvingdebrisdiscsinterrestrialplanetregionswithMIDI-VLTI

RachelSmith (KeeleUniversity)with M.C. Wyatt(IoA UniversityofCambridge), and C.A. Haniff

(CavendishLaboratory, UniversityofCambridge)

DustinmostdebrisdiscsoriginatesinplanetesimalbeltsakintotheKuiperbeltat> 30AU fromtheirstars. Relativelyfewstarsexhibitdustat < 30AU.BecauseofthesmallspatialscalesinvolvedadirectdeterminationofthediscmorphologyinsuchregionsrequirestheuseoflongbaselineinterferometrywithinstrumentssuchasMIDI ontheVLTI.InthistalkwepresentMIDI observationsoffourdebrisdisctargetswithdustbelievedtolieintheterrestrialplanetregions(∼ 1AU).Theyouthoftwoofthesetargets(12-16Myr)meansthattheobserveddustcouldbeindicativeoftheon-goingformationofterrestrialplanets. Fortheremainingtwooldertargets(1.3-2Gyr)thedustislikelytobeindicativeofarecenttransientevent. WediscussthelimitswecanplaceonthediscstructurewiththeMIDIobservations, andhowtheselimitscanbeinterpretedwithindifferentmodelsforthedustorigin.

CharacterisingtheconvectionpatternonBetelgeuse

JohnYoung (UniversityofCambridge)withA. Chiavassa, X. Haubois, E. Pedretti, B. Plez,

E. Josselin, G. Perrin, and B. Freytag

TheredsupergiantBetelgeuse(AlphaOrionis)isanirregularvariablestar. Betelgeuseisthoughttoexhibitlarge-scaleconvectiveprocessesthatareimportantdriversofthevariabilityandmasslossfromthestar. Wereportnewmodellingofhigh-angularresolutionobservations, primarilyfromtheCOAST andIOTA interferometers, spanningseveralobservationepochsandmultiplewavebandswithintheI andH photometricbands.Theinterferometricobservables(visibilityamplitudesandclosurephases)arecomparedwithad-hocmodelsfortheapparentbrightnessdistributionandwith3D hydrodynamicsimulationsobtainedwithCO5BOLD,post-processedusingtheradiativetransfercodeOPTIM3D.Wefindthatthe3D simulationsareabletomatchtheobservedwavelength-dependenceoftheasymmetricbrightnessdistributionatallofthethreeepochstested,althoughtheapparentstellardiameterinbandpasseswithmoderateTiO opacityis5-10%largerthanpredictedbythesimulations. Hencewehaveconfirmedthepresenceofagranulationpatternfeaturingsmalltomediumscale(5–15mas)convection-relatedsurfacestructuresandalarge(∼ 30 mas)convectivecell.

P23A NanoflareDistributionGeneratedbyRepeated

RelaxationsTriggeredbyKinkInstabilityMichaelBareford (TheUniversityofManchester)

with Philippa Browning, andRonaldVander Linden

Itisthoughtlikelythatvastnumbersofnanoflaresoccurringinthesolaratmosphereareresponsibleforthecoronahavingatemperatureofmillionsofdegrees. WeproposethatsuchindividualheatingeventcanbetriggeredwhenacoronalloopbecomesunstabletoanidealMHD kinkmode. Afeatureofthemodelisthatitpredictsheatingeventswitharangeofsizes, dependingonwheretheinstabilitythresholdforlinearkinkmodesisencountered. Dissipationoftheloop'smagneticenergythroughfastmagneticreconnectionbeginsduringthenonlinearstageoftheinstability, whenlocalisedfragmentarycurrentsheetsform.

Theloopisrepresentedasastraightline-tiedcylinderwithzeronetcurrent. Thetwistinginducedbyrandomphotosphericmotionsarecapturedbytwoparameters, representingtheratioofcurrentdensitytofieldstrengthforspecificregionsoftheloop. Onsetofinstabilitycanthusbemappedasaclosedthresholdinthe2dimensionalparameterspace. Afterflaring, theloopevolvestothestateoflowestenergywheretheratioofcurrenttofieldisconstantandhelicityisconservedinaccordancewithRelaxationTheory. Weconsiderthattheloopundergoesrepeatedepisodesofinstabilityfollowedbyrelaxation, orthattheinstabilityandrelaxationtakesplaceinanensembleofsimilarloops; hence,afrequencydistributionofeventsizes(nanoflares)iscollated. Here, themodelisextendedtomuchmorerealisticconfigurationswhichcorrespondtolocalisedphotospherictwisting, andhencehavezeronetcurrent(contrastingwithpreviousworkinwhichtheloophadanetcurrent). Weshowthe

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resultsobtainedfromusingtwomethodsofcurrentneutralisationthatarecompatiblewithanon-zeromagneticflux. Theseresultsarecomparedwiththoseoftheearlierstudy.

Comparisonofmodelsoffluxtransfereventformationusingpredictedandobserved

asymmetryRobertFear (UniversityofLeicester)with

Steve Milan, Joachim Raeder, and David Sibeck

Fluxtransferevents(FTEs)areburstsofmagneticreconnectionataplanetarymagnetopauseandhavebeenobservedatEarth, JupiterandMercury.Theyareusuallyidentifiedbybipolarsignaturesinthecomponentofthemagneticfieldnormaltothemagnetopause(Bn). SeveralconceptualmodelshavebeenproposedforFTE formation, includingmodelsbasedonreconnectionatasinglereconnectionline(X-line)andatmultipleX-lines.Two-dimensionalmagnetohydrodynamicmodelshavepreviouslybeenusedtosimulatebothscenariosandhavefoundatendencyforFTEsgeneratedbysingleX-linereconnectiontoexhibitanasymmetryintheBnsignature, withtheleadingpeakbeingsubstantiallysmallerinmagnitudethanthetrailingpeak. Ontheotherhand, FTEsimulationsfeaturingmultipleX-linereconnectionledtomoresymmetricsignatures. WepresentacomparisonofthesesimulationresultswithobservationsmadeattheEarth’smagnetopausebytheClusterspacecraft, usingadatasetof213FTEswhichwereobservedbyallfourspacecraftin2002/3. A tendencyisfoundfortheBnsignaturestobeasymmetric, butwiththeleadingpeakstrongerthanthetrailingpeak- oppositetothepredictionmadebythe2D models. Wealsocomparetheobservationswiththeresultsofamorerecentglobal3D MHD simulationandfindsimilartrendstothoseobservedbyCluster.

TurbulentrelaxationofbraidedmagneticfieldsGunnarHornig (UniversityofDundee)withAnthony Yeates, Antonia Wilmot-Smith, and

David Pontin

Magneticbraidingofcoronalloopsduetothemotionoftheirphotosphericfootpointshaslongbeendiscussedasapossiblemechanismfortheheatingofthesolarcorona(E.Parker, 1972). Thismotivatedaseriesofnumericalexperiments(Wilmot-Smithetal. 2009, 2010)ontheturbulentrelaxationofbraidedmagneticfields. TheseexperimentshaveproducedrelaxedstateswhichdifferdrasticallyfromthepredictionsoftheTaylorhypothesis.

Wepresentanewtopologicalmeasure, atypeofgeneralisedfluxfunction, whichallowsustoanalysetherelaxationprocessandwhichshowsthattherearefurtherconstraintsontherelaxationprocessbeyondtheconservationofthetotalhelicity, whichpreventthesystemfromrelaxingtoaTaylorstate.

3-D MagneticreconnectionatseparatorsClareParnell (UniversityofStAndrews)with

Andrew Haynes, and Rhona Maclean

Magneticseparatorsarespecialfieldlinesthatconnecttwomagneticnullpointsandlieontheintersectionofthesurfacesmadeupoffieldlinesthatextendfromthenullpoints. Three-dimensionalreconnectioncanoccurinmanylocationsincludingnullpoints, separatrixsurfacesandseparators. Weconsidertheimportanceofseparatorreconnectionbyconsideringvarious3DresistiveMHD experimentsinwhichreconnection

isakeyprocess. Inparticular, wediscussthefrequencyofoccurrenceofseparators, theirbehaviourandthenatureofreconnectioninthevicinityofaseparator. WewillconcludebyindicatingtheconsequencesofseparatorreconnectionfortheSun.

A surveyofHXR emissionofseismicallyactiveandquietX-classwhite-lightflares

EhsanPedram (UniversityCollegeLondon–MSSL)with Sarah Matthews

Sun-quakes, generatedduringtheimpulsivephaseofsomesolarflares, arethemostintenseacousticradiationobservedonthesolarsurfaceandofferinterestingpossibilitiesforfurtheringourunderstandingofflaresandactiveregionhelioseismology. Variousmechanismshavebeenproposedastohowseismicwavescanbegeneratedfromasolarflare. Recentworkhasshownaclosecorrelationbetweenenhancedcontinuumemissionandtheseismicemissionobservedduringtheimpulsivephase. InthisstudywehaveexaminedtheHXR emissionfromYohkohandRHESSI togetherwithwhitelightemissiondataobservedbyGONG andTRACE.Highrateofenergydepositionandtheareaoverwhichtheenergyisbeingdepositedonsuggestsback-warmingasaplausiblemechanismforgeneratingsun-quakes. Combiningthisresultwithspatialandtemporalcorrespondenceofwhite-lightemissionwiththepeakintensityofHXR emissionfurtherenhancesthispossibilitywhichisinagreementwithfindingsofpreviousstudies.

Regimesofmagneticreconnectionat3D nullpoints

DavidPontin (UniversityofDundee)withE.R. Priest, and K. Galsgaard

Magneticreconnectionat3D nullpoints-- aswellastheseparatrixandseparatorstructuresassociatedwiththem-- isthoughttobeofgreatimportanceintheSolarcorona. Ourunderstandingofthereconnectionprocessesthatmayhappenatnullshascomealongwayinrecentyears, althoughmanyopenquestionsremain.Recentadvancesintheoryandcomputationalexperimentshaveshowntheneedtorefinethepreviouscategorisationofmagneticreconnectionatsuch3D nulls. Wepresenthereanewcategorisationintothreebasicmodes, dependingonthenatureoftheflownearthespineandfanofthenull. Wewilldiscussthebasicpropertiesofthesethreereconnectionmodes- 'spinefanreconnection', 'torsionalspinereconnection'and'torsionalfanreconnection'. Particularemphasiswillbeplacedonthemostcommon'spine-fan'reconnectionmode, inwhichthenullpointlocallycollapsesformingacurrentsheetspanningboththespineandfan, andresultingintransportofmagneticfluxacrossboththefanandspine.

Doesmagnetichelicityeffectactiveregionevolutionandenergetics?

AlisonWallace (UniversityCollegeLondon–MSSL) with LucieM. Green, SarahA. Matthews,

Cristina Mandrini, Pascal Demoulin, andLidiavan Driel-Gesztelyi

ThepuposeofthisstudyistoinvestigatetheinteractionsbetweensameandoppositehelicitystructuresincludinglargescalereconnectioneventssuchasflaresandCMEs, aswellassmallscaleevents. Ofthesetwoscenarios, theonethatproducesthemostenergyisstillatopicfordebate.Wepresentobservationsoftwoactiveregionsfollowingtheemergenceofabipole, onewiththe

sameandonewiththeoppositesignofhelicityfromtheactiveregion. InbothcasesnewfluxemergedattheNorth-Westernedgewithinthenegative(leading)polarity. Thelifetimeofthefirstbipolewas37hrsandthecounter-helicitybipolewas67hrs. Wediscusstheroleofreconnectioninre-distributinghelicityandhowthiseffectstheactiveregionevolution.

Relaxationofbraidedcoronalloopsbymultiplesmall-scalereconnectionevents

AntoniaWilmot-Smith (UniversityofDundee)withDavidI. Pontin, Gunnar Hornig,

AnthonyR. Yeates, and Klaus Galsgaard

Braidingofthesolarcoronalmagneticfieldisaprimecandidateforcoronalheating. Wereassessmagneticbraidingwithparticularemphasisonrecentdevelopmentsin3D magneticreconnectiontheory, concentratingontheevolutionoftheintegratedparallelelectricfield, acrucialquantityfor3D reconnection.

Westartwitharealisticbraidednon-linearforce-freemagneticfieldwithzerototalmagnetichelicity. ThefieldisnotinresistiveMHDequilibriumandwetrackthelossofstabilityandsubsequentdynamicsviaanumericalsimulation.Strongcurrentconcentrationsareformedintheearlyevolution, thelocationofwhichisgovernedbyregionsofinitiallyhighintegratedparallelelectricfield.

Subsequentlythefieldundergoesaturbulentrelaxation, evolvingintotwounlinkedforce-freefluxtubes. Detailsofthereconnectionprocessesduringrelaxationareexamined; magneticfluxisfoundtoevolveinacomplexmannerandisreconnectedmultipletimes. TheendstateoftherelaxationsuggestsasegmentedTaylor-likeprocesstakesplaceandthatadditionalconstraintsbeyondtheconservationoftotalhelicitygoverntherelaxation. Someprogresstowardsdeterminingtheseconstraintsisreported.

PropertiesoftheDistributionFunctionofaVlasov-MaxwellEquilibriumfortheForce-Free

HarrisSheetFionaWilson (UniversityofStAndrews)with

Thomas Neukirch, and Michael Harrison

A discussionispresentedofaVlasov-Maxwellequilibriumrecentlydiscoveredfortheforce-freeHarrissheet. Fortheforce-freeHarrissheet, forcebalanceismaintainedbyamagneticshearfieldinsteadofagradientoftheplasmapressure, theplasmapressurebeingconstantalongwiththedensityandthemagnitudeofthemagneticfield.Thedistributionfunctionrecentlyfoundfortheforce-freeHarrissheethasanumberofinterestingproperties, whichvarywithparametervalues. Forexample, thedistributionfunctioncanbemulti-peakedintwoofthevelocitydirections, whichmayhaveimplicationsfortheonsetofmicro-instabilities.

3D MagneticNullpoints: LocalisedFantiltingandTorsionalReconnection

PeterWyper (Sheffield)with Rekha Jain

MagneticReconnection, aprocessofbreakingideal- MHD frozen-in-fluxconstraintsonfieldlineconnectivity, isbelievedtobeanefficientmechanismforheatingthesolarcorona. Theprocessisofgreatimportanceinmanyotherastrophysicalandlaboratoryplasmas. Themagneticfieldintheseplasmascanbeverycomplexwiththreedimensional(3D) structure.

74 P23

Reconnectionleadstoarearrangementofthemagnetictopologyandareleaseofstoredmagneticenergyinsuchstructuresifthefieldlinesaretwistedorsheared. Itcanalsoreleaseenergyandaccelerateparticleswherelargegradientsofthemagneticfielddevelop, forexamplemagneticnullpoints. Recenttheoreticalprogressinourphysicalunderstandingofthe3D nullpointreconnectionhasbeentoexaminemagneticfluxandplasmaflowsacrosstheFanandSpineandtounderstandtheirtimeevolution. Inthistalk, wewilldiscussthreetypesofsecondaryreconnectionarounda3D nullpointfromananalyticalstandpoint: Fantilting/distortion, TorsionalspineandTorsionalfan.

P24TheHeliophysicsIntegratedObservatory

RobertBentley (UniversityCollegeLondon–MSSL) with Mike Hapgood, Chris Perry,

John Brooke, AnjaLe Blanc, Kevin Benson, andVineeth Shetty

TheHeliophysicsIntegratedObservatory, HELIO,iscreatingacollaborativeenvironmentwherescientistscandiscover, understandandmodeltheconnectionbetweensolarphenomena,interplanetarydisturbancesandtheireffectsontheplanets. HELIO willprovideintegratedaccesstodatafromthesolar, heliospheric, geophysicsandplanetarydomainsandallowtheusertoundertakeasearchforinterestingeventsandphenomenabasedsolelyonmetadataanddataproducts.

WewilldescribehowHELIO canbeusedtoaddressscienceproblemsthatspanthedomainsbyallowingtheusertotrackphenomenaastheypropagatethroughthesolarsystem.

TheHELIO infrastructureisbeingdevelopedaroundaservice-orientedarchitecture. Thesearchforinterestingeventsandphenomena, andthetaskofthenfindingandretrievingthedatahasbeensplitintoanumberofservicesthatcaneitherbeusedindependentlyoraspartofaworkflow.

VersionsofsomeoftheHELIO servicesarestartingtobecomeavailableandwearelookingforuserthatcanhelptestandrefinetheseandassistinthetaskofdefininguserinterfacesthatbettermatchtheneedsoftheresearchcommunity.

HELIO isaresearchinfrastructurefundedunderCapacitiesprogrammeoftheEC's7thFrameworkProgramme(FP7); theprojectstartedinJune2009andhasadurationof36months. TheHELIOConsortiumincludesthirteengroupsfromtheUK,France, Ireland, Italy, Switzerland, SpainandtheUS.

A ComprehensiveStudyofthe13-15May2005SolarEvent(s)

MarioBisi (AberystwythUniversity)withA.R. Breen, B.V. Jackson, R.A. Fallows, A.P. Walsh,

M.J. Owens, Z. Miki, P. Riley, C.J. Owen,A. Gonzalez-Esparza, A.G. Wood, E. Aguilar-

Rodriguez, H. Morgan, E.A. Jensen, M. Tokumaru,P.K. Manoharan, K. Fujiki, I.V. Chashei,A.S. Giunta, J.A. Linker, V.I. Shishov,

S.A. Tyul’bashev, G. Agalya, S.K. Glubokova,P.P. Hick, J.M. Clover, B. Pintér, and A. Buffington

Wepresentanoverviewoftheresultsofamulti-technique, multi-instrument, co-ordinatedstudyofthesolar-eruptiveeventof13May2005anditsprogressionthroughtheinnerheliosphere. We

havecombinedobservationsandmeasurementsfromcoronalandinterplanetaryremote-sensinginstruments, interplanetaryandnear-Earthin-situmeasurements, remote-sensingobservationsandin-situmeasurementsoftheterrestrialmagnetosphereandionosphere, alongwithcoronalandheliosphericmodelling. WediscusstheresultantEarth-directed(halo)coronalmassejection(CME),andbriefly, theeffectsontheterrestrialspaceenvironmentandupperEarthatmosphere. Theseanalysesareusedtotracetheorigin, development, propagation, terrestrialimpact, andsubsequentconsequencesofthiseventtoobtainthemost-comprehensiveviewofageo-effectivesolareruptiontodate. FulldetailsofthestudyofthiseventcanbefoundinBisietal.,SolarPhysics, TopicalIssue(TI) onRemoteSensingoftheInnerHeliosphere, 2010, whentheTI ispublished.

AssessingtheaccuracyofCME speedandtrajectoryestimatesfromSTEREO observationsthroughacomparisonofindependentmethodsChristopherDavis (STFC RutherfordAppletonLaboratory)with J.A. Davies, and J. Kennedy

WehaveestimatedthespeedanddirectionofpropagationofanumberofCoronalMassEjections(CMEs)usingdatafromtheSTEREOHeliosphericImagers. Ingeneral, thesevaluesareingoodagreementwiththosepredictedbyThernisienetal(2009)usingaforwardmodellingmethodtofitCMEsintheSTEREO COR2coronagraphdata. ThereissomeevidencefromthissurveythatthespeedofaCME ismodulatedbytheambientsolarwindspeed. Thetechniquewasverifiedbyin-situdatawherepossible. WealsoshowthattheuncertaintiesinourderivedparametersareinfluencedbytherangeofelongationsoverwhicheachCME istracked. Inordertoreducetheuncertaintlyinthepredictedarrivalat1AU towithin6hours, aCME needstobetrackedouttoatleast30degreeselongation.SuchatechniqueallowsthepredictionofEarth-directedCMEstobemadelonginadvanceoftheirarrival, providingapotentialadvanceinspace-weatherforecasting.

PropagationofanEarth-DirectedCoronalMassEjectionin3D

PeterGallagher (TrinityCollegeDublin)withJasonP. Byrne, ShaneA. Maloney, and R.T. James

McAteer

Wehavedevelopedanewmethodtoreconstructthe3D evolutionofaCME frontusingtheSunEarthConnectionCoronalandHeliosphericInvestigation(SECCHI) onboardtheSolarTerrestrialRelationsObservatory(STEREO).On12December2008anEarth-directedCME wasobservedbySTEREO whilethespacecraftwereinnearquadratureat86.7ºseparation. ThispositioningpresentsanidealcaseforobservingitspropagationthroughthecombinedSECCHIinstrumentfields-of-viewandapplyingourtechniquetoreconstructtheCME frontin3D.ThereconstructionallowsustodeterminethetrueCME frontkinematicsandmorphology, andwemeasurethreeimportantdynamiceffectsatplay:deflectionfromahighlatitudesourceregion; anincreasingangularwidth; andinterplanetarydrag.

SolarStormwatch: acrowd-sourcingapproachtounderstandingCoronalMassEjections

MarekKukula (RoyalObservatoryGreenwich)withChris Davis, Chris Lintott, and Natasha Waterson

TheSolarStormwatchprojectisanewonlineinitiativewhichmakesuseofthelargearchiveofdatafromtheSTEREO missiontogainadeeperunderstandingoftheoriginandpropagationofCoronalMassEjections. SolarStormwatchispartofthenewwaveof“crowdsourcing”or“citizenscience”projectswhichenlistmembersofthepublictohelpcarryoutresearchwhichcouldnotbedonebyscientistsworkingalone. Thespacecraftdataarepresentedinanappealingandaccessiblewaywhichisheavilyinformedbythedesignofpopularonlinegames. Thewebsiteincludestutorialsectionswhichallowinteresteduserstofindoutmoreaboutsolarphysicsaswellasasectionforschoolswithsuggestionsforclassroomactivities. Howeverthesciencegoalsaregenuineandwillleadtousefulandsignificantresearchoutput. Aswellascarryingoutrigorousanalysisofanotherwiseunder-utiliseddataset,userscanparticipateinavibrantonlinecommunitywhichincludesscientistsfromtheSTEREO mission. ExperiencewithpreviouscitizenscienceprojectssuchasGalaxyZooshowsthatasignificantsubsetofuserswilleducatethemselvestothepointatwhichtheyareabletospotunusualphenomenaandbringthesetotheattentionofthescienceteam, raisingtheprospectofentirelyunexpectedandnoveldiscoveries. TheprojectisaninitiativeoftheRoyalObservatory, GreenwichinpartnershipwiththeRutherfordAppletonLaboratoryandtheCitizenScienceAlliance. Assuch, itharksbacktotheprominentrolewhichtheObservatoryplayedinsolarphysicsinthe19thandearly20thcenturies.

Probingtheevolutionofcoronalandheliosphericstructureswithsuprathermalelectrons

MathewOwens (UniversityofReading)withNancy Crooker, Nathan Schwadron, Tim Horbury,

Benoit Lavraud, and Alexis Rouillard

Thedistributionandevolutionofmagneticfluxatthephotosphereiscomplex. Itisdominatedbymid-latitudemagneticfluxemergence, whichsubsequentlymigratestothepoles, ultimatelyfacilitatingthesolarcyclepolarityreversal. Thisismorphologicallydifferenttothefieldreversalobservedintheheliosphere, whichproceedsasasimplerotationofanapproximatelydipolarfield.Themagnetically-dominatedcoronalinksthesetwodisparateregions, thoughtheprocessesresponsibleforthenecessarysolarcyclerestructuringofthecoronaarenotwellunderstood. Ithasbeensuggestedthatcoronalmassejections(CMEs)playacriticalroleincoronalreconfiguration, bysheddingexcesshelicity, addingfluxtotheheliosphereandtransportingopenfluxinthemannerrequiredforthesolarcyclepolarityreversal. Suprathermalelectronobservationsprovideameanstotesttheseideas. I’llpresentasummaryoftheseobservationsandattempttointerprettheminthewidercontext.

Investigatingtheobservationalsignaturesofmagneticcloudsub-structure

KimberleySteed (UniversityCollegeLondon–MSSL) with C.J. Owen, P. Demoulin, and S. Dasso

Magneticcloudsareasub-setofinterplanetarycoronalmassejections(ICMEs)thatexhibitamagneticfluxropestructure. Theyareoftenprimarilyidentifiedbysmooth, large-scalerotationofthemagneticfield, howeverbothsmalland

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large-scalefluctuationsofthemagneticfieldareobservedwithinsomemagneticclouds. Wehaveidentifiedasmallnumberofmagneticcloudswithinwhichmultiple, small-scalereversalsofthegradientoftheazimuthalmagneticfieldareobservedtowardstheircentres, andwehereinusetheterm'sub-structure'torefertotheregionsthatexhibitthissignature.

On13April2006, amagneticcloudwasobservedbyACE andWindwhichdisplaysmanyofthetypicalcharacteristicsusedtoidentifyamagneticcloud, andalsoexhibitstheclearestexampleofsub-structuretowardsitscentrethatwehavefound. Investigationsofthemagneticfieldobservationsthatcharacteriseamagneticcloudcontainingsub-structureandassociatedchangesintheplasmaobservationshaveshownthatthemagneticstructuredoesnotevolveoverashorttimescaleoftheorderofafewminutes, andthatthismagneticcloudissubjecttocompression,probablyasaresultofthefastsolarwindstreambehindit, whichisparticularlystronginthesub-structureregion. Wesuggestseveralpossibleexplanationsforsub-structurewithinmagneticclouds, includingthepresenceofmultiplefluxropes, warpingofthemagneticcloudstructureandinsitumagneticreconnection.

Smallscaletransientfeaturesatcoronalholeboundaries: apossiblesourcefortheslowsolar

wind?SrividyaSubramanian (ArmaghObservatory)with

M.S. Madjarska, and J.G. Doyle

Coronalholesareregionsofpredominantlyunipolarcoronalmagneticfieldswithasignificantcomponentofwhichisopenintotheheliosphere.Ouraimwastofurtherexplorethesmall-scaleevolutionofCH boundariesusinghigh-resolutionandhigh-cadenceimagesfromtheX-raytelescope/HinodetakenwithanAlPolyfilter. WeidentifiedtransientX-raybrighteningsinequatorialcoronalholes, polarcoronalholes, andthequietSunwithandwithouttransientcoronalholesusinganautomatedidentificationprocedure. WefoundthatincomparisontothequietSun, theboundariesofcoronalholesareabundantwithbrighteningeventsincludingareasinsidecoronalholeswhereclosedmagneticfieldstructuresarepresent. ThestatisticalinvestigationofX-raybrighteningsshowedthataround70%ofthemincoronalholesandtheirboundariesshowexpandingloopstructuresand/orcollimatedoutflows, whileonly30%inthequietSunshowoutflowswithmostofthemappeartobecontainedinthecoronabyclosedmagneticstructures. WesuggestthattheejectedplasmaguidedbytheopenmagneticfieldlinesincoronalholesandtheirboundariesescapestheSuncontributingtotheslowsolarwind.

CharacterisingtheSTEREO HeliosphericImagersignaturesofCorotatingInteractionRegions

AnthonyWilliams (UniversityofLeicester)withS.E. Milan, J.A. Davies, C.J. Davis, and

R.A. Harrison.

DuringthecourseoftheSTEREO missionveryfewcoronalmassejectionshavebeenobserved, evenfewerhavebeenobservedtobeEarth-directed.Despitethis, theHeliosphericImagers(HI) detectastampedeofoutward-propagatingcoronalplasmaenhancements, indicatingstructuredsolarwindoutflow. A widelyreportedmethodofestimatingthespeedanddirectionfromelongation-time(J-)mapsoftransienteventswhichallowsthepredictionofthetime-of-arrivalofthese

featuresatEarth. Whilethismethodisreportedtoworkwhencomparingtimesofarrival, itfrequentlyappearstoproducespeedsfarlowerthanthespeedswhentheyareeventuallydetectedbyin-situspacecraftsuchasACE.TobetterunderstandthenatureofthesesignaturesweinterpretfamiliesoftracesasoriginatingfromasinglecoronalholeboundaryonthesurfaceoftheSungivingrisetoacorotatinginteractionregion(CIR).WesuccessfullyshowacorrespondencewithassociatedCIR signaturesobservedatACE,anddissecttheanatomyofaCIR asseenbyHI.Theseresultshighlightthedifficultyofinterpreting2D imagesofthe3D heliosphere, whenthereareoftenwithmanysimultaneousactiveregionsandoverlappingheliosphericstructuresalonganyparticularline-of-sight. WeoutlinestrategiesforthefutureinterpretationofHI images.

Non-potentialenhancementoftheSun'sopenmagneticflux

AnthonyYeates (UniversityofDundee)withD.H. Mackay, and A.A. vanBallegooijen

Formingafundamentaldynamicalconnectionwiththeheliosphere, theSun'slarge-scalemagneticfieldisshapedbyinteractionsinthelowercorona(belowabout2.5solarradii).Traditionalmodelsfortheglobalmagneticstructureinthisregionhaveusedpotentialfieldsourcesurface(PFSS) extrapolationsfromphotosphericmagneticobservations. However, insituspacecraftmeasurementsoftheinterplanetarymagneticfieldoverseveralsolarcyclesshowthatthePFSS extrapolationspredicttoolowalevelofopenmagneticfluxduringepochsofhighersolaractivity. Herewesuggestthatthisdiscrepancymayberesolvedbyrelaxingthepotential-fieldassumptionandallowingforelectriccurrentsinthelowcorona. Wedemonstratetheconceptusingaquasi-staticnumericalmodelofthelarge-scalecoronalmagneticevolution, whichsystematicallyproducesthesecurrentsthroughfluxemergenceandshearingbysurfacemotions.Thecurrentsinflatethemagneticfield, enhancingtheopenfluxduringperiodsofhighersolaractivity, inagreementwithIMF observations. Inaddition, theejectionofmagneticfluxropesinthemodelmimicstheeffectofcoronalmassejectionsthatcauseshort-termfluctuationsintheheliosphericmagneticfield.

Arethereimprintsofhotplasmaoutflowsfromactiveregionsinthesolarwind?

LidiavanDriel-Gesztelyi (UniversityCollegeLondon–MSSL) with A.N. Fazakerley, and

L.K. Harra

HinodehasdiscoveredapotentialsourceofsolarwindattheedgesofactiveregionswithXRT andEIS (e.gSakaoetal., 2007, Harraetal., 2008,Doscheketal., 2008). Theseoutflowsarelong-lastingandexistattheedgesofmostactiveregions. WehaveexaminedinterplanetarysolarwinddatafromtheACE spacecraftandsolarremotesensingdataincludingEIS plasmaupflows,duringafullCarringtonRotationinterval. WediscusswhethertheevidencesupportstheideathattheflowsthatweseeonthesurfaceoftheSunactuallyaretransportedtotheEarthinthesolarwind, orifitsuggeststhattheyaremerelyrelatedtoflowsinlarge-scaleloops.

P25FindingtheSourceofUHECRsusingBayesian

AnalysisofPierreAugerDataLauraWatson (ImperialCollege, London)with

Andrew Jaffe, Daniel Mortlock, and Roberto Trotta

Cosmicraysareextremelyenergeticparticlesandmustoriginatefromsomeofthemostenergeticprocessesinnature. DeterminingtheirorigincouldshedlightonprocessesthatplayakeypartintheUniverse'sevolution. Itissuspectedthatultrahighenergycosmicrays(UHECRs)maycomefromactivegalacticnuclei(AGNs): statisticalanalysesofthecorrelationbetweenthelocationofAGNsandUHECR detectionsweremadepossibleforthefirsttimebyobservationsfromthePierreAugerobservatory(PierreAugerCollaboration,Science318, 938, 2007). However, whilstthesefindingshinttowardscorrelation, amorerecentanalysishasfoundaweakenedcorrelation(Nature463, 1011, 2010). Herewepresentacompletelydifferentapproachtotheproblemwhichtakesthefullamountofavailableinformationintoaccount.ThroughBayesiananalysis, weprovideamethodforfindingtheprobabilitythatUHECRsoriginatefromAGNsanddiscusstheextensionofthismethodtothecomparisonofdifferentsources.

P26Globalpopulationstatistics, bimodalityand

multivariatedistributionsofgalaxieswithSDSS.IvanBaldry (LiverpoolJMU)

TheSDSS increasedthenumberof z < 0.2

galaxieswithknownredshifts, spectralandmulti-colourmeasurements, byanunprecedentedfactoroverthecourseofafewyears. Thishasledtoanexplosioninstudiesoftheglobalpopulationstatisticsofgalaxies. Thedangerintheseanalysesisthatimportantdetailsarelost, ontheotherhand, theycanprovidestrongconstraintsongalaxyevolutionandtheyprovideadescriptionofourUniverseonatrulycosmicscale. I willreviewsomeoftheSDSS resultsobtainedusingglobalpopulationstatisticsincludingthesignificantcolourbimodalityandenvironmentaltrends.

Whitedwarfsastracersofstellar, binary, andplanetaryevolution

BorisGaensicke (UniversityofWarwick)

I willreviewthetremendousimpactthattheSloanDigitalSkySurveyhashadonourunderstandingofawidevarietyofastrophysicalenvironmentscontainingwhitedwarfs. Besidesincreasingthetotalnumberofknownwhitedwarfsmorethanfive-fold, allowingdetailedstudiesoftheirgalacticpopulation, SDSS hasfoundnew, rarebreedsofwhitedwarfsthattraceextremebranchesofstellarevolution. SDSS hasalsoprobedthepopulationsofaccretinganddetachedwhitedwarfbinariestoanunprecedentedlevelofdetail, providingthemoststringenttestsofbinaryevolutiontodate. Atotallyunexpecteddiscoverywastheidentificationofplanetarydebrisdiscsaroundwhitedwarfs,originatingfromthetidaldisruptionofrockyasteroids. Assuch, thesesystemsofferaglimpseintothedistantfutureofourownSolarsystem,and, moregenerally, provideinsightintothelateevolutionofplanetarysystems.

76 P24–P26

EvidenceofTidalStrippingofthreecompactelliptical(cE) galaxiesdiscoveredinSDSS DR7

AvonHuxor (UniversityofBristol)withS. Phillipps, J. Price, and R. Harniman

Wepresentthreecompactgalaxies, foundinasearchofSDSS DR7, whichexhibitclearevidenceoftidalsteams. Thegalaxiesarelowmass, andhavesmalleffectiveradii, andtheirspectraindicatethattheypossessyoungtointermediate-agestellarpopulations. TheseprovidedirectevidencefortheprocessoftidalstrippingthatisbelievedtobetheoriginofM32-typegalaxies, a"smokinggun". Thesecompactgalaxiesareallfoundinsmallgroups, suggestingthatwemaybeseeingtheformationofsuchgalaxiesindynamicallyyounggalaxygroupings. OneofthethreeisfoundinasmallgroupnotunliketheLocalGroupitself, andthusprovidesanadditionalmodelforunderstandingM32.

GalaxyClusteringintheSDSSJonLoveday (UniversityofSussex)

I willreviewwhatwehavelearntaboutgalaxyclusteringfromtheSDSS,includingconstraintsontheHaloOccupationDistribution(HOD)formalism, therelativeclusteringofgalaxiesofvaryingcolourandluminosity, andthefirstandsubsequentdetectionsoftheBaryonAcousticPeakinthegalaxydistribution.

DVORAC Detector- TheDurhamVOronoiRed-sequenceAutomatedClusterDetectorfornext-

generationpanoramicsurveysDavidMurphy (DurhamUniversity)with

Jim Geach, and Richard Bower

WepresenttheDVORAC detector, anewclusterdetectionalgorithmdesignedforlargepanoramicsurveyswithmulti-bandphotometry. Themethodmakesnopriorassumptionsonthepropertiesofclustersotherthan(a)thesimilarityincolourofclustergalaxies(theredsequence)and(b)alargeprojectedsurfacedensity. Thedetectorhastwomainstages. First, itidentifiesclustermembersbyphotometricallyfilteringtheinputcataloguetodetectover-densitiesincolour-magnitudespace.Second, aVoronoitessellationidentifiesregionsofhighsurfacedensityandgroupsgalaxiesintoclusters. Asthenextgenerationofsurveysprobetofainterlimits, quickandefficientalgorithmswillberequiredtohandlethevastvolumesofdatagenerated. ToprepareforthePanoramicSurveyTelescopeandRapidResponseSystem(PanSTARRS) survey, wehavetestedthedetectorontheSDSS Equatorial"Stripe82", andamockMediumDeepSurvey(MDS) PanSTARRScataloguebasedonthe ΛCDM modelwithasemi-analyticgalaxyformationrecipe. WewillshowthatclustersdetectedintheSDSS showgoodagreementwithexistingclustercataloguesandthatthebenefitofdeeperdatahasallowedustoidentifymanypreviouslyundetectedclustersandgroups. Themocksurveyhasallowedustoquantifytheefficiency, robustnessandreliabilityofthealgorithmbycomparingthecatalogueofdetectedclusterstothemembershipofgalaxiesindarkmatterhaloes.

AnalysingtheClusteringofPhotometricallySelectedGalaxies

AshleyRoss (UniversityofPortsmouth)withWillJ Percival, and RobertJ. Brunner

TheSDSS hasproducedphotometricredshiftcatalogswhichcontainover20milliongalaxies.Wehavecreatedofapproximatelyvolumelimited

samplesofthesegalaxies, allowingprecisemeasurementsoftheangular2-pointcorrelationfunctionofgalaxies. Splittingthesegalaxiesintoredshiftshellsbetweenz=0.1and0.4, wehavefoundasignificantincreaseinthebiasof L*galaxiesbetweenz=0.1and0.4. Usingthemeasurementstodeterminethethehalo-occupation-distribution(HOD) ofthegalaxiesineachredshiftshell, wefindourmeasurementscanbeexplainedbytheformationof L*galaxiesinhalosofmass ∼ 1012h−1M⊙. Whenwesplitthegalaxiesbytype, wefindthat, inordertoself-consistentlyfitthemeasurements, early- andlate-typegalaxiesmustpreferentiallyexistinseparatedarkmatterhalos.

TheSDSS-III BaryonOscillationSpectroscopicSurvey(BOSS):FirstResults

NicholasRoss (LawrenceBerkeleyLab)withErinS. Sheldon, AdamD. Myers,

Christophe Yeche, and SDSS-III:BOSS Team

TheSDSS-III (www.sdss3.org)BaryonOscillationSpectroscopicSurvey(BOSS) isanewfive-yearproject, whichcommencedoperationsinlate2009. ThekeygoalsofBOSS aretomeasureredshiftsfor1.4millionLuminousRedGalaxies(LRGs)to z < 0.8, andsimultaneously160,000quasarsat z > 2.2. Bothsampleswillmeasuretheequationofstateofdarkenergyto1%usingtheBaryonAcousticOscillation(BAO) technique.HerewedescribethesomeoftheveryearlyresultsfromtheBOSS CommissioningPhasewhichtookplacein2009andearly2010.

Higher-OrderClusteringOfLuminousRedGalaxiesInTheSDSS

CristianoSabiu (None)with Robert Nichol, andFelipe Marin

TheSloanDigitalSkySurvey(SDSS) LuminousRedGalaxy(LRG) spectroscopicsampleprovidesuswithamapoflarge-scaleover- densitiesintheUniversewithinavolumeof ∼ 1 (Gpc/h)3. ThemainadvantageofusingLRGsisthattheyarehighlybiasedwithrespecttotheunderlyingdarkmatterandthusefficienttracersofthelarge-scalestructuresintheUniverse, e.g., LRGshavebeenessentialforthedetectionandmeasurementoftheBaryonAcousticOscillations(BAO).TomakefulluseoftheLRG samples, itisimportanttoaccuratelymodelthemappingbetweengalaxiesandthedarkmatter. Recently, thishasbeenachievedusingthe"halomodel"forhowgalaxiesinhabittheirdarkmatterhalos. Indetail, weusetheHaloOccupationDistribution(HOD) topopulateasuiteofN-bodysimulations(tocreateagridofmockcatalogues), andcomparethesetotheobservedLRG population. Toaddconstrainingpower, weusetheThree-PointCorrelationFunction(3PCF),whichencodesmuchmoreinformationthantheusualtwo-pointstatistics. Inthistalk, wepresentresultsofourHOD analysisforanLRG sampleselectedfromthefinalDR7SDSS catalogue.

SDSS-II SNe- AnOverviewandHostGalaxyProperties

MathewSmith (UCT) with R. Nichol, H. Lampeitl,B. Dilday, B. Bassett, and SDSS-II SNeSurvey

Team

MeasurementsoftypeIaSupernovaehaverevolutionisedthecosmologicalmodelthroughtheintroductionofDarkEnergy. TheSDSS-IISupernovaSurveyspectroscopicallyidentifiedover500oftheseeventsatintermediateredshift(0.05 < z < 0.5)andobtainedhighqualitylight-

curvesforhundredsmore. BycombiningtheseSNeIa'swiththosefromothersurveys, themostaccuratemeasurementsofthecontentoftheUniversehavebeenmade. Weshalldescribethesurveyitself, it'sdeterminationofthecosmologicalparametersandinvestigatetherelationshipthatthesecosmologicalprobeshavewiththeirlocalenvironment. BycreatingarobustandrepresentativesampleofSNeIa'swehaveshownthattheseeventsarefarmorelikelytoappearingalaxieswithrecentstar-formationactivitythan"passive"galaxies, andthattheSNeIarateisstronglydependentonhostgalaxystar-formationrate. Additionally, weshowthatthereisanenvironmentdependenceofthestretchdistributionsoftheseevents, andintriguinglythatSNeindifferentenvironmentsmaypossessdifferentabsolutemagnitudesanddifferentdustlaws.

DiscoveryofthefirstwideL dwarf+giantbinarysystemandeightotherultra-cooldwarfsinwide

binariesZengHuaZhang (UniversityofHertfordshire)withDavid Pinfield, Avril Day-Jones, Ben Burningham,

and Hugh Jones

Weidentify806ultra-cooldwarfsfromtheirSDSSrizphotometry(ofwhich34arenewlydiscoveredL dwarfs)andobtainpropermotionsthroughcrossmatchingwithUKIDSS and2MASS.Propermotionanddistanceconstraintsshowthatnineofourultra-cooldwarfsaremembersofwidelyseparatedbinarysystems; SDSS 0101(K5V+M9.5V),SDSS 0207(M1.5V+L3V),SDSS0832(K3III+L3.5V),SDSS 0858(M4V+L0V),SDSS0953(M4V+M9.5V),SDSS 0956(M2V+M9V),SDSS 1304(M4.5V+L0V),SDSS 1631(M5.5V+M8V),SDSS 1638(M4V+L0V).Oneofthese(SDSS 0832)isshowntobeacompaniontothebrightK3giantEtaCancri. Suchprimariescanprovideageandmetallicityconstraintsforanycompanionobjects, yieldingexcellentbenchmarkobjects. EtaCancriAB isthefirstwideultra-cooldwarf+giantbinarysystemidentified. WepresentnewobservationsandanalysisthatconstrainthemetallicityofEtaCancriA tobenearsolar, anduserecentevolutionarymodelstoconstraintheageofthegianttobe2.2- 6.1Gyr. IfEtaCancriBisasingleobject, weestimateitsphysicalattributestobe: Mass = 63 − 82MJup,Teff = 1800 ± 150 K, log g = 5.3 − 5.5,[M/H] = 0.0 ± 0.1. Itscoloursarenontypicalwhencomparedtootherultra-cooldwarfs, andwealsoassessthepossibilitythatEtaCancriB isitselfanunresolvedbinary, showingthatthecombinedlightofanL4+T4systemcouldprovideareasonableexplanationforitscolours.

BinarypopulationsinSDSS:A newdiagnosticforsystemparametersofevolvedwhitedwarf

binariesLiekevanSpaandonk (UniversityofWarwick)with

D. Steeghs, and T.R Marsh

EvolvedbinarysystemsformalargesubsetofbinarystarsandCataclysmicVariables(CVs)areavaluablesamplewithinthisgroupastheyprovidehomogeneousconfigurationsofwhitedwarfsplusnearmain-sequencemassdonors. A keyexpectationbasedonourcurrentunderstandingofbinaryevolutionisthatangularmomentumlossdrivesCVstoshortorbitalperiodsastheirmassdonorstarsshedmass. Theyprovidethesettingforthestudyofaccretionontocompactobjects,includingTypeIasupernovaeandgravitationalwaveemission. However, theseshort-period

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systemsarefaintandthereforesampleshavetraditionallybeenbiasedagainstthem.

ThishasfinallychangedthankstoCV searcheswithinSDSS astheyareunearthingshort-periodsystemsinlargernumbers. Althoughtheorbitalperiodisanimportantdiagnostic, reliablemassestimates(e.g. massratio q = Mdonor/MWD)areneededforthedonorstarstoplaceaCV onitsevolutionarytrack.

Wehavestudiedpromisingcandidatesatthebrightendoftheshort-periodbinarysample,exploitingtheCaII tripletlinesinordertorecovertheirbinaryparameters. TheCaII linesofferadvantagesoverthehydrogenandheliumlinescommonlyused, asthelatteraredominatedbybroadaccretiondiscprofiles. Ourdatasofarclearlyvindicatethisstrategy, asmostsystemsrevealsharpemissionfromtheintrinsicallyfaintdonorsontopofthediscemission, allowingustodeterminethebinaryparametersinsystemssuchasrevealedbySDSS.

P27TheLastMajorEpochofDiskGrowthinM33MichaelBarker (RoyalObservatoryEdinburgh)with A. Ferguson, R. Ibata, M. Irwin, G. Lewis,

T. Smecker-Hane, and N. Tanvir

Late-typediskgalaxieslikeM33arecommoninthenearbyuniverse, butdifficulttoproduceincosmologicalsimulations, soabetterobservationaldeterminationoftheirevolutioniscrucialforunderstandingdiskformation. Tothatend, weuseHubbleSpaceTelescopeAdvancedCameraforSurveysimagingtostudythestarformationhistory(SFH) oftwofieldsat9.1and11.6kpcalongM33’snorthernmajoraxis. Basedonthedistributionofstarsinthecolour-magnitudediagrams, wefindthatthemajorityofstarsinbothfieldsformedat z < 1. Themeanageoftheinnerfieldis ∼ 3 Gyrandthemeanageoftheouterfieldis ∼ 6 Gyr. TheseresultsofferthemostdetailedviewyetofM33’speripheryandprovideamuch-neededobservationalconstraintonthelastmajorepochofdiskassemblyinthisgalaxy.

BPASS:BinaryPopulationandSpectralSynthesisJohnEldridge (InstituteofAstronomy(Cambridge))

with Elizabeth Stanway, Norbert Langer,Monica Relano, and Christopher Tout

Thereisgrowingobservationalevidencethatthebinaryfractionofmassivestarsisclosetounity.Thereforetomodelyoungstellarpopulationsaccuratelythecomplexandnon-linearevolutionofbinariesmustbeincluded. Wehavecreatedapowerfulanduniquebinarypopulationandspectralsynthesiscode, BPASS,thataccountsforbinaryevolutionbyusingthousandsofdetailedbinarystarmodelsincreatingsyntheticstellarpopulation(Eldridge&Stanway, 2009,MNRAS,400, 1019). Wediscusstheimportantdifferencesthatwefindbetweensinglestarandbinarypopulationsforvariedobservablesofresolvedandunresolvedstellarpopulations. Wealsoshowhowthesedifferencesgrowasthemetallicityofthestellarpopulationdecrease.

DependingontimewewillalsodiscoverhowwearetestingandcalibratingBPASS bystudyingsystemssuchasNGC604inM33thatareresolvedbyHST butunresolvedbyothertelescopessothatwecanhavegreaterconfidenceinBPASS when

applyingittostudyingthestellarpopulationsofhigh-redshiftgalaxies.

ConstrainingtheInitialMassFunctionIgnacioFerreras (UniversityCollegeLondon–

MSSL) with Dominik Leier(ARI,Heidelberg), andPrasenjit Saha(Zurich)

TheInitialStellarMassFunction(IMF) remainsoneofthemainunknownsinsyntheticmodelsofstellarpopulations. ThemassiveendoftheIMFcanbeconstrainedviastudiesofopenclustersandyoungpopulations. However, thelow-massendoftheIMF ismuchhardertoconstrainduetothelowluminosityofstarsbelow1Msun. AlternativemethodsestimatingthetotalmassareneededtosetconstraintsonthelowerendoftheIMF.InthistalkI willpresentrecentworkfocusedontheEinsteinCross. A non-parametricanalysisofthelensingsystemiscomparedwithpopulationsynthesismodels. A combinationofhighresolutionimagingwithHST/NICMOS anddeepspectroscopywithVLT/FORS givesM/L predictionsthatarecomparedwithanumberofpopulationsynthesismodelsforarangeofIMFs. I willalsopresentpromisingnewmethodsbasedonmulti-variateanalysistoconstraintheIMF fromspectroscopicdataofunresolvedstellarpopulations.

KinematicbiasinexoplanetsurveysRichardHutcheon (KeeleUniversity)with

P.F.L. Maxted

Over400exoplanetsarenowknown, discoveredmainlybythetransitorradialvelocitymethods.FromthesesystemsweselectaBrightTransitSample(BTS) andaRadialVelocitySample(RVS).Duetoobservationalconstraintsthedistancesofstarsinthesesampleslieinalmostnon-overlappinggroups, furtherorcloserthan100pcfortheBTS andRVS respectively. Sincethetransitsurveysavoidlowgalacticlatitudes, theBTS starstendtoliefurtherfromtheGalacticplane. Wehaveinvestigatedwhetherthesebiasesareexpectedtointroducedifferencesinthedistributionofageormetallicity, parameterswhicharethoughttoinfluencethefrequencyofexoplanets.

TheaverageandmedianmetallicitiesoftheRVSarerespectively0.03and0.10dexhigherthanfortheBTS.Calibrationsamplesofsolar-typestarswithsimilarkinematicstotheBTS andRVS starshavebeenpreparedandtheseshowamedianmetallicity0.02dexhigherfortheRVS.Thecalibrationsamplesarelargeenoughtorevealevensmalldifferencesbetweenthem. Henceanydifferenceinmetallicitiesisverysmallandisduetokinematics. Themetallicitiesoftheactualsamplesareabout0.2dexhigherthanforthecalibrationsamples; thisconfirmsearlierresultsthatplanethoststarsaremetal-richcomparedwithothersolar-typestars. ThereisnosignificantdifferencebetweentheagesofthestarsintheBTSandRVS samplesortheircalibrationsamples, butthisismostlyduetothelargeuncertaintyinestimatingtheagesofmain-sequencesolartypestars.

Weconcludethattheselectioneffectsinherentinthetransitsurveyandradialvelocitytechniquescan, inprinciple, leadtodifferentbiasesinthemetallicityandagedistributionsofthestarsobservedbutthisdifferenceappearstobenegligibleinpractice.

Crystallinesilicatesaroundoxygen-richAsymptoticGiantBranchStarsintheLarge

MagellanicCloudOliviaJones (UniversityofManchester)with

F. Kemper, B.A. Sargent, G.C. Sloan, P.M. Woods,A.K. Speck, M. Matsuura, J.-P. Bernard,

K.D. Gordon, R. Indebetouw, K.E. Kraemer,E. Lagadec, J. Th. vanLoon, I. McDonald,

M. Marengo, M. Meixner, W.T. Reach, andA.G.G.M. Tielens

Ithasbeenshownthatthesilicatesinthedustshellsaroundoxygen-richstarsontheasymptoticgiantbranch(AGB) canshowaconsiderabledegreeofcrystallinity. A thresholdvalueforthemass-lossrateexists, abovewhichthefeaturesduetothecrystallinesilicatesforsteriteandenstatiteappear. Weareinvestigatingtheoriginofthisthresholdvaluebyexpandingthecrystallinitystudiestothemetal-poorenvironmentoftheLargeMagellanicCloud(LMC).WepresentSAGE-SpecSpitzer-IRS spectroscopyforanumberofO-richAGB starsintheLMC.The5-40micronspectraoftheseevolvedO-richobjectsencompassarangeofspectralfeaturesandbandstrengths; fromthespectrallyrichwhichexhibitawealthofcrystallineandamorphoussilicatefeaturestothe`naked'(dust-free)stars, acrossarangeofmass-lossrates,providinganidealopportunitytoexploretheonsetofcrystallinity. Wemeasuredthefeaturestrengthofcrystallinesilicatebandsat23.6, 28, 33.6 µm,withrespecttothestrengthofthecontinuumproducedbythermalemissionfromamorphoussilicates. WeintendtoplotthesevaluesagainstMdust and Mgas, inordertosearchforacorrelationwiththedustandgasdensityrespectively. TheserelationsmaybedifferentattheLMC'smetallicityof ∼ 0.5 Z⊙. WecompareourresultstothoseforO-richAGB starsintheGalaxy.

Theroleofminormergersinthestarformationhistoryofearly-typegalaxies

SugataKaviraj (ImperialCollegeLondon)withRichard Ellis, Sukyoung Yi, Kevin Schawinski,

Joseph Silk, GALEX Collaboration, and MUSYCCollaboration

Anexcitingrecentdiscoveryhasbeenthedetectionofwidespreadrecentstarformation(RSF) innearbyearly-typegalaxies(ETGs), usingnewsurveydataintherest-frameUV.Wereviewthecurrentstatusofthiswork, withaparticularemphasisonthedriversofthisstarformation.DatafromtheGALEX UV survey(z < 0.1),combinedwithdeepopticalsurveys(e.g. MUSYC,GOODS,COSMOS) thattracetherest-frameUVathighredshift, indicatethatETGsofallluminositiesformstarsoverthelifetimeoftheUniverse, withluminoussystems(−23 < MV < −21)formingupto10-15%oftheirstellarmassafterz=1. WhilesmallmassfractionsofyoungstarsseemtobeubiquitousinthenearbyETG population, thesourceofthisstarformationremainsamatterofdebate. WedemonstratethattheRSF atlateepochscannotbedrivensolelybyinternalmassloss, suggestingthatsomeormostofthegasfuellingtheRSF isexternallyaccreted. VisualinspectionofHSTimagesofETGsfromtheCOSMOS surveyatz∼ 0.5 showaremarkablecorrespondencebetweenthepresenceofmorphologicaldisturbancesandUV excess, whichsuggeststhatmergersmaybetheprincipaldriverofthisRSF.However, themajormergerrateisfoundtobetoolowtosatisfythenumberofETGsthatcarrysuchmorphologicaldisturbances, suggestingminormergersastheprimarychannelofgasaccretionandstarformationintheETG population. We

78 P27

discusstheimplicationsofrepeatedminormergeractivityonthespectralanddynamicalevolutionofmassivegalaxiesanddrawcomparisonswiththeliteraturewhichsuggestthatminormerging, ahithertopoorlyexploredprocess, maybeakeyelementoftheevolutionofgalaxiesatlateepochs.

Systematicuncertaintiesinherentinstellarpopulationsynthesismodelsandtheirimpacton

integratedspectraofstellarpopulations: Amodeller'sperspective.

SusanPercival (LiverpoolJohnMooresUniversity)

Stellarpopulationsynthesismodelsareavitaltoolforinterpretingthepropertiesofstellarpopulations(age, metallicity, SFH) inbothstellarclustersandgalaxies. ErrorsonthesederivedpropertiescanstemfromsystematicuncertaintiesintheSPSmodelsthemselves, and/orfromcertainpropertiesinherentinthestellarpopulationwhichcancomplicatetheinterpretationofresults. Allstellarpopulationsynthethismodelsrelyoncalibrationsofthe3mainstellarparameters- effectivetemperature, surfacegravityand[Fe/H].Thesescalesareimplicitinstellarmodels, isochronesandsyntheticspectra, andareexplicitlyadoptedforempiricalspectrallibraries. InthistalkI willdiscusstheeffectofamismatchinscalesbetweenisochronesandspectrallibraries(thetwokeycomponentsofSPS models)anddemonstratetheimpactongalaxyagesandabundanceratiosderivedfromcommonlyuseddiagnosticlineindices, andfromfullSED fitting. I willalsobrieflydiscusstheeffectofextendedbluehorizontalbranchesandstatisticalfluctuationsonthederivedpropertiesofstellarclusters.

TheAGB populationandthemetallicitygradientinNGC 6822

LisetteSibbons (UniversityofHertfordshire)withMaria-Rosa Cioni

NGC 6822isasmallIrregulardwarfthatformspartofthelocalgroup. Itscloseproximity(∼ 470

kpc)andapparentisolationprovideauniqueopportunitytostudygalacticevolutionwithoutstrongdynamicalfactors. ThisprojectaimstostudythemetallicitygradientandthedistributionofthestellarpopulationwithinNGC 6822viatheasymptoticbranchstar(AGB) componentofthestellarpopulation. Usingdeephighqualitynear-infraredphotometry, takenusingUKIRT in2008,thecarbon- andoxygen-richintermediate-ageAGB starshavebeenisolated. Theratiobetweenthesepopulations, theC/M ratio, hasthenbeenusedtoderivethe[Fe/H] abundancewithinthegalaxy. The[Fe/H] abundanceandthedistributionoftheAGB populationwerethenanalysedasafunctionofgalacticradius. Usingcolour-magnitudediagramsthetipoftheredgiantbranchstarshasbeenlocatedatKs=17.29±0.03andthecolourseparationforC- andM-typestarsfallsatJ-K =1.188±0.01. UsingthesecutsearlyresultsindicateanoverallC/M numberratioof0.248,withvariationinthenorthandsouth, aswellasatlargergalactocentricdistances. AlsoadenserAGBpopulationhasbeenlocatedintheSW regionofthegalaxyinthedirectionoftheouterspheroid.Summarizing, theresolvedAGB populationacrossthewholeofNGC 6822hasbeeninvestigatedandregionsofvaryingmetallicity, andAGB stellardensity, havebeenidentifiedwhichmayindicateachangeorsomepasteventinthestarformationhistoryofthegalaxy.

Learningaboutstellarpopulationsinunresolvedgalaxies

RussellSmith (DurhamUniversity)

I willreviewcurrenttechniquesforlearningaboutthestellarcontentofunresolvedgalaxies, throughintegrated-lightspectroscopy. Thesemethodshavebecomeacrucialweaponintheobservationalastronomer'sarsenal, andarenowroutinelyappliedtosamplesrangingfromtensuptotens-of-thousandsofgalaxies, toconstrainthehistoryofstarformationandchemicalenrichmentinthedistantpast. Buthowdoweproperlyinterprettheresultsofsuchstudies? Howdowemakemeaningfulcomparisonstogalaxyformationmodels? Whathavewereallylearned? Whatarethecurrentlimitations, andaretheyfundamentalormerelypracticaldifficultiestoovercomewithlargertelescopesandcleverermodelling? I willelaborateonsomeofthesequestions, tostimulatediscussion, buttheycannotbeansweredinafifteen-minutetalk!

AGB StarsinWLMBejaminTatton (UniversityofHertfordshire)with

Maria-Rosa Cioni

Theaimofthisprojectistoinvestigatethestarformationhistoryandmetallicityofthelocalgroup, irregulardwarfgalaxyWLM (Wolf-Lundmark-Melotte).

ThemaindatausedforthisstudyiswidefieldJHKsnearinfraredimagingspanningaregionofapproximately1sq. degreeobtainedwiththeWideFieldCameraonUKIRT.

Colour-magnitudediagrams(J-KsvsKs)allowedforthedeterminationofthetipoftheredgiantbranchandfortheidentificationC-typeandM-typestarslocations. TheC/M ratiowasthencalculatedleadingtotheproductionofasurfacemapofmetallicitydistribution. Theseresultswerecomparedwithinformationintheliterature.

ThestellarpopulationsintheLargeMagellanicCloud

PaulWoods (UniversityofManchester)withSAGE-Specteam

I presenttheclassificationresultsofSAGE-Spectroscopy, aSpitzerLegacyprojectwhichobtainedIRS spectraofanumberofpoint-source-likeobjectsintheLargeMagellanicCloud(LMC).SuchasurveygivesusinformationaboutthedustcontentoftheLMC,andidentifyingthenatureoftheobjectsdetectedinthemid-IR helpsustounderstandhowthatdustiscycled. I willdetailtheobjectclassificationprocess, andtheresultswhichcanbedrawnfromsuchanendeavour. Wecanreliablydistinguishredsupergiantsfromoxygen-richAGB starsbymeansofcolour, andareabletotracetheevolutionofcarbon-richevolvedstarsbymeansoftheirdustcontent. Wealsofindthat(massive)youngstellarobjectsfallintooneoffourevolutionarygroupings.

P28Thedriftofauroralradioabsorptionpatches

observedbyimagingriometerJohnHargreaves (UniversityofLancaster)with

M.J. Birch, and B.J.I. Bromage

Thephenomenonofdriftingpatchesofauroralabsorption, firstrecognisedinthe1960s, ishere

illustratedinrecentobservationswithanimagingriometerinnorthernFinland. Possiblecausesareconsidered, usingincoherent-scatterobservationsfromEISCAT andF-regionvelocitiesfromSuperDARN.

MagneticfieldparallelcurrentsintheUCL-CTIPmodel

TimothySpain (UCL) with RichardB. Horne, andAlan Aylward

ThemagneticfieldparallelcurrentsintheEarth'sionospheredonotcontributetoeithertheiondragorJouleheatingofthethermosphere, duetothecross-productbetweenthetotalcurrentandthemagneticfieldintheseterms. Asaresult, thecalculationofthesecurrentswasneverexplicitlyincludedintheUCL-CTIP model, despitetheperpendicularcomponentsofthecurrentbeingcalculatedinaself-consistentmanner. Thecalculationofthefieldparallelcurrentcomponentallows, forexample, thecalculationofthetotalmagneticfieldbythepoloidal-toroidalmethod.HerewepresentamethodofcalculationofthefieldparallelcomponentofthetotalcurrentandanapplicationofthiscalculationtosomesimpleexperimentsperformedwiththeUCL-CTIP model.

ModellingGeomagneticallyInducedCurrentsintheNationalGridusingSAMNET.

KatieTurnbull (LancasterUniversity)withA.W.P. Thomson, C. Beggan, J.A. Wild, and

F. Honary

WepresentthefirstresultsofanewmodelwhichusesmagnetometerdatatocalculateGeomagneticallyInducedCurrents(GIC)throughouttheUK NationalGrid. GIC arearesultofrapidvariationsinthegeomagneticfield, suchasthoseobservedduringmagneticstormsandsubstorms. GIC cantravelalongpowertransmissionlinesasquasi-directcurrent,potentiallydamagingtransformersandresultinginblackouts.

ThenewUK modelusesSubAuroralMagnetometerNetwork(SAMNET) data, themethodofsphericalelementarycurrentsystemsona2D gridanda3D conductivitymodeloftheUK anditscontinentalshelftodeterminethesurfaceelectricfieldduringstorms. ThiselectricfieldisthenusedtocalculateGIC throughtheNationalGrid, throughthegroundingpointsofeachhighvoltagetransformerinthenetwork. WecomparemodelledGIC withmeasuredGIC duringoneparticularsubstormforfoursitesinScotland,aswellasdiscussingthemodelledGIC atsiteselsewhereintheNationalGrid. Infutureworkwewillexaminethegridresponseduringmajormagneticstorms, suchasthe'Halloween'eventofOctober2003.

P29A newenthalpy-basedapproachtothetransition

regioninanimpulsively-heatedcoronaPeterCargill (ImperialCollege)with

Steve Bradshaw

Observationsofthesolarcoronarevealpersistentandubiquitousred-shifts, whichcorrespondtobulkdown-flows. Foranimpulsively-heatedcorona(e.g. bynanoflares)thisindicatesthatamajorityofthecomponentloopstructuresareintheradiativelycoolingphaseoftheirlifecycle.However, thenatureofthebulkdownflowsraises

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thepossibilitythatenthalpymayplayakeyroleintheenergybalanceoftheloopsandinparticularthatitpowersthetransitionregionradiation. Weuseonedimensionalhydrodynamicsimulationsofloopcoolingtoshowthatenthalpylossesfromthecoronaareeasilysufficienttopowerthetransitionregionradiation. Thiscontrastswiththelong-heldviewthatdownwardthermalconductionpowersthetransitionregion. Thetraditionaldistinctionbetweenthetransitionregionandthecoronaintermsoftemperaturealoneisthenagrosslyunphysicalsimplificationandaproperdefinitionoftheinterfacebetweentheseatmosphericlayersrequiresadetailedknowledgeoftheirenergybalance. Tothisendweproposearobustnewdefinitionofthetransitionregion.

Chromosphericmagneticreconnection:implicationsforjet-likeeventsandcoronal

heatingJiaoyangDing (ArmaghObservatory)withM.S. Madjarska, J.G. Doyle, and Q.M. Lu

Magneticreconnectioninthelowatmosphere,e.g., chromosphere, isinvestigatedinvariousphysicalenvironments. Itisfoundthatthetemperatureandvelocityoftheoutflowjetsasaresultofmagneticreconnectionarestronglydependentonthephysicalenvironments, e.g. themagnitudeofthemagneticfieldstrengthandtheplasmadensity. Thestrongermagneticfieldstrengthorthelowermassdensityis, theoutflowjetswithhighertemperatureandlargervelocityareobtained. Undercertainphysicalconditions,theoutflowjetscanbeheatedupto 2 × 106 K(coronaltemperatures), anditsmaximumvelocityreaches300- 400km/s. Inthiscase, bothcoldchromosphericjetsandhotcoronaljetsareobtainedsimultaneously. Thisisveryhelpfultounderstandtherelationshipbetweencoldandhotjets, aswellascoronalheatingmechanisms.

Observationand3D modellingofacoronalbrightpoint

ZhenghuaHuang (ArmaghObservatory)withM.S. Madjarska, K. Galsgaard, and J.G. Doyle

Weusemulti-wavelengthobservationsobtainedwithEIS,XRT andSOT onboardHinodetostudytheplasmapropertiesanddynamicsofacoronalbrightpointobservedinanequatorialcoronalhole. Theevolutionofthebrightpointwasfollowedinspectrallineswithformationtemperaturesfrom 104 K to 2 × 106 K,i.e. fromchromospherictocoronaltemperatures. Wefoundthatthebrightpointhasalongerlifetimeasseeninlowerchromospherictemperaturesthaninhigher,coronalones. WederivedthedensityevolutionofthebrightpointusingthespectrallineratioFeXII186/195. Weobtaineddensitieswhichfluctuateintherangefrom 8 × 108 to 3 × 109 cm−3 withanaverageofabout 2 × 109 cm−3. ThetimesequenceofXRT imagestakenwiththeAlpolyfilterwerealsousedtostudythedynamicsofthebrightpoint. Theplasmapropertiesofthebrightpointwillbecomparedwiththeoutputfroma3DMHD simulation. The3D modelisacombinationofastratifiedhydrostaticmodelatmosphereandapotentialmagneticfieldthatisobtainedusingpotentialmagneticfieldextrapolationfromlongitudinalmagnetogramfromSOT observations.ThemagneticstructureisstressedbyimposingaphotosphericvelocityflowderivedfrombluecontinuumSOT datausingballtracking.

CalculationandapplicationofR-matrixelectron-impactexcitationdataforionsofinterestto

astrophysicaldiagnosticmodellingGuiyunLiang (UniversityofStrathclyde)with

N.R. Badnell

A largenumberofhigh-resolutionandhigh-qualityspectrahavebeen, andcontinuetobe,obtainedfromboththeEUV (e.g. Hinode)andX-ray(e.g. Chandra, XMM-Newton, IXO) regions.Manyemissionlinesobservedinthesespectraarepotentialdiagnosticsoftheelectrontemperatureanddensityofcoronal-likehotplasmas. Therearealsomanyunidentifiedemissionlinesandlargediscrepanciesinlineintensityratioslikelyduetounknowncontaminants. Suchdiagnosticsandassociatedlineidentificationsrequireaccurateatomicdata, especiallyforelectron-impactexcitation.

Theadvantagesoftheintermediate-couplingframetransformationR-matrixmethod(Griffinetal.1998)makeitfeasibletoprovideexcitationdataalongK- andL-shelliso-electronicsequencescoveringasubstantialrangeofastrophysicallyimportantionsatthehigh-levelofaccuracyaffordedbythe R-matrixmethod. ThisisoneofthekeygoalsoftheUK AtomicProcessesforastrophysicalPlasmas(APAP) network. HerewewilladdresseffectivecollisionstrengthsalongtheNe-likeiso-electronicsequence(Liang&Badnell2010). Wealsolookataparticularion-Fe13+

(Liangetal. 2010)forwhichalaboratorymeasurementhasbeenmade. Weassesstheaccuracyofourexcitationdatainbothcases.

Usingthelatest R-matrixelectron-impactexcitationdata, weanalyzetheEUV andsoftX-rayspectraofhotplasmas, e.g. stellarcoronaandelectron-beamion-traps. SeveralpreviousquestionablelineintensityratiosinFe13+ havebeenexplainedsatisfactorilyandsomelinesareidentifiedinastrophysicalsourcesforthefirsttimewiththeaidofalaboratorymeasurementperformedattheHeidelbergEBIT (Liangetal.2010).

PlasmapropertiesofanX-rayjetfrommulti-instrumentco-observations: SUMER/SoHO,

EIS/XRT/HinodeandEUVI/SECCHI/STEREO AandB

MariaMadjarska (ArmaghObservatory)

Wewillpresentuniquemulti-instrumentobservationsofanX-rayjet-likeeventtakenwithSUMER/SoHO,EIS/XRT/HInodeandEUVI/SECCHI/STEREO.Thephenomenonaroseinacoronalbrightpointsituatedattheboundariesofanequatorialcoronalhole. Thecombinationoftwospectrometerscoveringtogetherthetemperaturerangefrom10000K to12MK andthethreeviewpointsofXRT,EUVI A andBpermittedustoderivetheplasmapropertiesanddynamicsofthisfeature. Weanalysedthebehaviourofdifferentspectrallinesduringthemicro-flaringwhichtriggeredthejet-likeevent.Wealsoobtainedthetemperaturesanddensitiesinthereconnectionsiteandthesurroundingregion.Thejetdynamicsanditsplasmapropertieswillbediscussedindetail. Wewillgiveoursuggestionsforthefutureinstrumentation(spectroscopicandimaging)andatomiccalculations.

AlfvénIonisationintheSolarPhotosphereProchetaMallik (UniversityofGlasgow)with

DeclanA. Diver, Lyndsay Fletcher, HughE. Potts,and CraigS. MacLachlan

Strongphotosphericflowsnearactiveregionsinevitablyinvolvemixingneutralgasand

magnetisedplasma. Wheretherelativespeedbetweenneutralandplasmaspeciesexceedsacriticalvalueatwhichtheenergyintheflowisequaltothefirstionisationpotentialofacomponentspecies, thatspecieswillbeionised.Thephysicalmechanismisasfollows: theneutralgasimpingingontheplasmacollideswiththepositiveionsanddisplacesthem, causingpocketsofnegativechargeimbalance. Theresultingelectricfieldsaccelerateatailofelectronstoenergiesabovetheionisationthresholdforparticulargasspecies. Thesenewionsremaintrappedinthemagneticstructure, leadingtoenhancedabundanceinthelowersolaratmosphere. Wepresentnumericalsimulationsoftheevolutionoftheelectrondistributioninsuchasituation, showinghowafractionoftheaffectedpopulationreachesenergiesabovetheionisationthresholdforparticularelements. Thisismostrelevantforlowcriticalionisationvelocity(CIV)elementssuchasXe, K,Cr, Mn, Feetc, andisakeydriverofelementover-abundance.

Non-LinearForce-FreeModeloftheSolarMagneticCarpet

KarenMeyer (UniversityofStAndrews)withD.H. Mackay, and A.A. vanBallegooijen

WemodelthedynamicalevolutionoftheSun'smagneticcarpet, andconstructanon-linearforce-freecoronalfieldbasedonsurfacemotions.Ratherthanindependentlyextrapolatingthecoronalfieldateachtimestep, wemodelacontinuousevolutionofthefieldthroughamagnetofrictionalrelaxationtechnique. Sofarwehavestudiedenergybuildupwithinthefieldduetothebasicinteractionsofcancellation,emergenceandflyby. ThemagnetofrictionalcodehasalsobeendirectlyappliedtoHinode/SOTmagnetogramdatatostudythelocationandvariationoflowcoronalnullpoints.

Detailedobservationsandmodellingofasmallflare

UrmilaMitraKraev (UniversityofCambridge(DAMTP)) with G. DelZanna, H. Mason,

S.J. Bradshaw, and A. Asai

Wehaveobtainedaplethoraofspatially- andtemporally-resolvedspectraldataofaB-classflarewiththeEIS spectrometeron-boardtheHinodesatellite. TogetherwithdatafromtheotherHinodeinstruments, aswellasGOES,TRACE andtheNobeyamaRadioHeliograph, adetailedpictureoftheevolutionofthisflareisputtogether. Theflareshowsmany'typical'featuressuchasprecursorevents, brighteningsintheribbons, andhot(10MK) emissionandsubsequentcooling. However,anumberoffeaturesarenew, suchasstrongblue-wingasymmetriesonlyseeninlinesformedbetween1.5and2.2MK.ThetemporalandtemperaturecoverageoftheEIS observationsprovidesnewinsightsintoourunderstandingofchromosphericevaporationandcooling. AnumericalsimulationusingtheHYDRAD codetostudythecoolingofthe10MK plasmaisingoodagreementwiththeobservations. Lineblendinginsomepotentiallyusefullinesforflarediagnosticsisalsodiscussed.

Theopticaldepthofwhite-lightflarecontinuumHughPotts (UniversityofGlasgow)with

Hugh Hudson, Lyndsay Fletcher, and Declan Diver

Thewhite-lightcontinuumemissionofasolarflareremainsapuzzleasregardsitsheightofformationanditsemissionmechanism. Thiscontinuum, anditsextensionintothenearUV,containthebulkof

80 P29

theenergyradiatedbyaflare, andsoitsexplanationisahighpriority. Wedescribeamethodtodeterminetheopticaldepthoftheemittinglayerandapplyittothewell-studiedflareof2002July15, makinguseoftheMDI intensityimages. Theopticaldepthofthevisiblecontinuuminthisflareissmall, consistentwiththeobservationofBalmerandPaschenedgesinotherevents.

Whatblinkersactuallyare?SrividyaSubramanian (ArmaghObservatory)with

M.S. Madjarska, J.G. Doyle, and D. Bewsher

Weinvestigateblinkersinanequatorialcoronalholeregionusingspectral, imagingandmagnetogramco-observationstofindoutwhattheseblinkersactuallyrepresent. WeusedanautomatedidentificationproceduretoidentifyblinkersinSoHO/CDS O v629Angstromrasters.WealsoidentifiedbrighteningsinSTEREO/EUVIFeIX 171AngstromimagesandHinode/XRT Alpolyimagestostudyblinkersatlowercoronaltemperaturesandtofindtheirpossiblecoronalcounterparts, respectively. AllCDS blinkershadEUVI 171Å counterparts. Identifiedblinkereventswereclassifiedintotwogroups, blinkerswithcoronalcounterparts, mostlyassociatedwithcoronalX-rayjets, andblinkerswithnocoronalcounterpartswhichappearaspointedbrighteningsattransitionregiontemperatures. Thelattercouldbesignatureofchromosphericfeatures(spiculesor/andmacrospicules)reachingtransitionregiontemperaturesorsimplyrepresentinducedflowsalongsmallscaleloopstructures. WebelievethatblinkersaretransientEUV responseofvariousdynamiceventsoriginatinganywhereinthesolaratmospherewhichcontributetothetemperatureraiseinthetransitionregion.

TheHydrodynamicEvolutionofImpulsivelyHeatedCoronalLoops: ExplicitAnalytical

ApproximationsDavidTsiklauri (QueenMaryUniversityof

London)with M.J. Aschwanden

Wederivesimpleanalyticalapproximations(inexplicitform)forthehydrodynamicevolutionoftheelectrontemperature T (s, t) andelectrondensity n(s, t), forone-dimensionalcoronalloopsthataresubjecttoimpulsiveheatingwithsubsequentcooling. Ouranalyticalapproximationsarederivedfromfirstprinciples,using(1)thehydrodynamicenergybalanceequation, (2)theloopscalinglawsofRosner-Tucker-VaianaandSerio, (3)theNeuperteffect,and(4)theJakimiecrelationship. Wecompareouranalyticalapproximationswith56numericalcasesoftime-dependenthydrodynamicsimulationsfromaparametricstudyofTsiklaurietal., coveringalargeparameterspaceofheatingrates, heatingtimescales, heatingscaleheights, looplengths, forbothfootpointandapexheating, mostlyapplicabletoflareconditions. Theaveragedeviationsfromtheaveragetemperatureanddensityvaluesaretypically ∼ 20%forouranalyticalexpressions.Theanalyticalapproximationsinexplicitformprovideanefficienttooltomimictime-dependenthydrodynamicsimulations, tomodelobservedsoftX-raysandextreme-ultravioletlightcurvesofheatedandcoolingloopsinthesolarcoronaandinflaresbyforwardfitting, tomodelmicroflares, toinferthecoronalheatingfunctionfromlightcurvesofmulti-wavelengthobservations, andtoprovidephysicalmodelsofdifferentialemissionmeasuredistributionsforsolarandstellarflares,coronae, andirradiance. M.J.Aschwanden, D.

Tsiklauri, Astrophys. J.Suppl. Ser., 185, 171-185(2009)DOI:10.1088/0067-0049/185/1/171

SpiculesandCoronalHeatingKamalamVanninathan (ArmaghObservatory)with

Maria Madjarska, and J.G. Doyle

Weusemulti-instrumentobservationsofspicules,lookingforevidenceofwhetherthesechromosphericfeaturescanalsobedetectedatcoronaltemperatures. WeanalysedCaII H imagesfromSOT/Hinode, comparingthemwithdatafromEIS/Hinode, plushigh-resolutiondatafromSUMER/SoHO.WeobservespiculesattheNorthpolewith10secondcadenceSOT data. A groupofrotatingspiculesasseenwithSOT areobservedintheSUMER transitionregionO V 629andN V1238asamacrospicule. EIS datadonotshowcorrespondingfeaturesatcoronaltemperatures.

MagneticreconnectionalongQSLs- amajordriverofactiveregionoutflows

LidiavanDriel-Gesztelyi (UniversityCollegeLondon–MSSL) with D. Baker, C.H. Mandrini,

and P. Demoulin

Therelationshipbetweenquasi-separatrixlayers(QSLs), orinthelimitofinfinitelythinQSLs,separatrices, andvariousactivityphenomenahasbeenexploredinmanydifferentsolarmagneticconfigurationsacrossallscalesinrecentyears. Intheabsenceofmagneticnulls, fastreconnectionalongQSLs, whicharespecificlocationsinthemagnetictopologywherefieldlinesdisplaystronggradientsofmagneticconnectivity, wasidentifiedasthemainphysicalprocessattheoriginofflares.Recently, itwasshownthatfast(tensofkm/s)persistenthotplasmaupflowsinactiveregions(ARs)canalsobelinkedtolocationsofQSLs. ItislikelythattheseupflowsthatoccurattheedgesofARsoverunipolarmagneticfieldconcentrationsareacceleratedbymagneticreconnectionalongQSLs. Wewillshowmulti-temperaturespectralscanobservationsfromHinode’sEIS combinedwithmagneticmodelingofQSLsintwoARsobservedon20-21February2007and11January2008. ThelatterAR isobservedandmodeledwhenitisinthevicinityofthesolarcentralmeridianwheretherearenoprojectioneffects,therebyeliminatingambiguitylinkingtheoriginofmulti-temperatureobservationsofAR upflowstoQSLs. WeusethePotentialSourceSurfaceModeltolookforopenfieldlinesinthevicinityofupflowsandQSL locationsinordertodemonstratewhethertheseupflowsbecomeoutflowsandcancontributetothesolarwind.

P30TheEffelsbergNorthernSkyPulsarSurvey

EwanBarr (MPIfR Bonn)

Pulsarsarerapidlyrotatingneutronstarswhichemitbeamsofbroadbandradioemissionfromtheirmagneticpoles. Theextremeconditionsfoundinandaroundpulsarsmakethemafantasticnaturallaboratorythroughwhichmanyaspectsoffundamentalphysicsandastronomycanbeprobed. Assuch, modernpulsarsurveysprovidethemeansthroughwhichwepavethewayfornewandexcitingscience. Whetheritisanexoticpulsarwhichpushesthelimitsoftheequation-of-state, ahighlyaccuratelytimingmillisecondpulsar(MSP) thatcanbeusedaspartofanarraytodetectgravitationalwavesoranormalpulsarthatwill

helpmaptheinterstellarmedium, thediscoveryofnewpulsarsinevitablyleadstoanimprovementinourunderstandingofoneormoreresearchareas.Thuswewillcommenceanorthernskyblindpulsarsurveywiththe100-mEffelsbergradiotelescopecomplimentedbyatwinsearchofthesouthernskywiththe64-mParkestelescope.

AlsopresentedhereisPSR J1745+1017,Effelsberg'sfirstevermillisecondpulsardetection,the18thradioFermipulsarsofardiscovered.

SurfaceextractionofelectronsinapulsarDeclanDiver (UniversityofGlasgow)with A.A. daCosta, E.W. Laing, C.R. Stark, and L.F.A. Teodoro

Wepresentanoveldescriptionofhowenergeticelectronsmaybeejectedfromthepulsarinteriorintotheatmosphere, basedonthecollectiveelectrostaticoscillationsofinteriorelectronsconfinedtomoveparalleltothemagneticfield.Thesizeoftheinteriormagneticfieldinfluencestheinteriorplasmafrequency, viatheassociatedmatterdensitycompression. Theplasmaoscillationsoccurclosetotheregionsofmaximummagneticfieldcurvature, thatis, closetothemagneticpoleswherethemajorityofmagneticfluxemerges. Giventhattheseoscillationshaveadensity-dependentmaximumamplitudebeforewave-breakingoccurs, suchwavescanejectenergeticelectronsusingonlytheself-fieldoftheelectronpopulationintheinterior. Moreover,photonsemittedbyelectronsinthebulkoftheoscillationcanescapealongthefieldlinesbyvirtueoftheloweropacitythere(andthefactthattheyareemittedpredominantlyinthisdirection),leadingtofeaturesinthespectraofpulsars.

GlitchesintherotationofPulsarsCristobalEspinoza (JodrellBankCentrefor

Astrophysics)with A.G. Lyne

A newsearchforglitcheswasperformedusingtheJodrellBankpulsartimingdatabase, and104newglitcheswerefoundintherotationof64pulsars.Combiningthesewiththosealreadypublishedwehaveputtogetheradatabasecontaining315glitchesin102pulsars. Thedatabasewasusedtostudytheglitchactivityamongthepulsarpopulation, findingthatitpeaksforpulsarswithacharacteristicage τ ∼ 10 kyranddecreasesforlongervaluesof τ , disappearingforobjectswithτ > 20Myr. Althoughtoalesserextent, theglitchactivityisalsolowerintheveryyoungpulsars(τ ∼ 1 kyr). Thecumulativeeffectofglitches, orthecolectionofmanyspin-upevents, actsagainsttheregularlong-termspindownrateofpulsars.Thepercentageofthespindownreversedbyglitchactivitywasfoundtovarybetween0.5%and1.6%forpulsarswithaspindownratebetween10−14 and 3.2 × 10−11 Hzs−1, decreasingtolessthan0.01%towardsbothhigherandlowerspindownrates. Theseratiosareinterpretedintermsoftheamountofsuperfluidinvolvedinthegenerationofglitches. Inthiscontext, theactivityoftheCrabpulsarmaybeexplainedbyquake-likeactivityonitscrust. Pulsarswithlowspindownratesseemtoexhibitmostlysmallglitches,matchingwellthedecreaseoftheamountofsuperfluidrelatedtoglitchactivity.

TheanalysisofglitchsizesindicatesthattheparticularglitchingbehaviourofPSR J0537-6910andtheVelapulsarmaybesharedbymostVela-likepulsars. Mostglitchesintheseobjectspresentthelargestfrequencyandfrequencyderivativejumpsrecorded, andseemtooccuratregularintervalsoftime.

P29–P30 81

A betterunderstandingoftheglitchingbehaviourofpulsarswillconductustowardsamorerefinedknowledgeofnotonlytheirinteriorsbutalsooftheirspinevolutionandgravitationalwaveemission.

Testsofgeneralrelativityandbinaryevolutionstudiesusingpulsarobservations

RobertFerdman (UniversityofManchester)

A briefreviewwillbegivenofseveralpredictionsofgeneralrelativity(GR) thatcanandhavebeentestedthroughtimingobservationsofpulsarsinbinarysystems. Thiswillcover, forexample,settinglimitsondipolargravitationalradiationandongravitationalconstantvariation, aswellasstrong-fieldtests. Alsotobediscussed, iftimepermits, isthestudyofbinarysystemevolutionusingpulsarobservations.

A BayesianSearchForGravitationalWaveRing-downsAssociatedWithPulsarGlitches

IkSiongHeng (UniversityofGlasgow)withJames Clark, Graham Woan, and Matthew Pitkin

Glitchesinpulsartimingarethoughttobeassociatedwithsuddenchangesinthepulsar'sangularmomentum. A fractionoftheexcessrotationalenergyisthenradiatedawayasgravitationalwaveemission. Wepresentasearchfordamped-sinusoidalgravitationalwaveringdownsusingBayesianmodelselection. Wedemonstratehowtheresultfromsuchasearchiseasilyconvertedintoastatementaboutthephysicalpropertiesofthegravitationalwaveemission.

CarbonatmosphereneutronstarinCassiopeiaA:YoungestneutronstarintheGalaxy

WynnHo (UniversityofSouthampton)withCraigO. Heinke

Thesurfaceofhotneutronstarsiscoveredbyathinatmosphere. Ifthereisaccretionafterneutronstarformation, theatmospherecouldbecomposedoflightelements(H orHe); ifnoaccretiontakesplaceorifthermonuclearreactionsoccurafteraccretion, heavyelements(e.g., Fe)areexpected. Despitedetailedsearches, observationshavebeenunabletoconfirmtheatmosphericcompositionofisolatedneutronstars. HerewereportananalysisofChandraobservationsoftheX-raysourceinthecentreoftheCassiopeiaAsupernovaremnant. Weshowthatacarbonatmosphereneutronstarproducesagoodfittothespectrum. Ouremissionmodel, incontrastwithothers, impliesanemissionsizeconsistentwiththeoreticalpredictionsfortheradiusofneutronstars. Thisresultsuggeststhatthereisnuclearburninginthesurfacelayersandalsoidentifiesthecompactsourceastheyoungest-known(withanageofabout330years)neutronstarintheGalaxy.

LatestHESS observationsofPulsarWindNebulaeDominicKeogh (DurhamUniversity)with HESS

Collaboration

Theconfinementoftherelativisticoutflowsofpulsarsproducesaluminouspulsarwindnebula(PWN) seenacrosstheelectromagneticspectrum.ThesesourcesareoneofthemostprominentclassesobservedbyTeV CherenkovobservatoriessuchastheNamibianbasedHESS telescopes.NumerousPWN havebeenobservedwithHESS,whileadditionaldarksourcesmayrepresentrelicPWN.InthistalkI shalloutlinesomeofthemostexcitingrecentobservationsofpulsarwindnebulaewiththeHESS telescopes.

TheopticalandinfraredcounterpartofSGR0501+4516

AndrewLevan (UniversityofWarwick)

I willpresentthediscoveryoftheoptical/IRcounterparttothesoft γ−repeaterSGR0501+4516. Unlikethemajorityofmagnetars,thisoneliesinthegalacticanticentredirection,andhasonlymoderateextinction, allowingustosearchforitscounterpartatlongerwavelengths.Ourcomprehensivecampaignofobservationsbeganonlyanhourafterthefirstactivationofthesource, andcontinuedfor14months. TheseobservationsrevealseveralcrucialdiagnosticsoftheIR counterpartofanSGR i)rapidoptical/IRvariabilityshowsaperiodalmostidenticaltotheX-rayderivedperiod(5.7s), ii)Thelongtermoptical/IR variationappearstotrackthatintheX-rayiii)Limitsonthepropermotionsuggestthatthespatialvelocityis < 400 km/s, andshowthatSGR0501+4516isnotassociatedwithanysupernovaremnants, oryoungstellarclusters, afirstforamagnetar.

Knownpulsarsascontinuousgravitationalwavesources

MatthewPitkin (UniversityofGlasgow)

Knownpulsarsareapotentialsourceofcontinuousgravitationalwavesandtherehavebeenongoingsearchesforthemwithincurrentgravitationalwavedetectordata. Nosignalshaveyetbeenseen, butbasedontheexpectedsensitivitiesoffuturedetectorsweexaminethepotentialfordetectingthem. Weexaminewhatkindofstar(e.g. strangequarkstar, hyperonstar,ornormalneutronstar)theseobjectswouldhavetobetoachievedetection. Wealsostudywhatdetectionscouldinferaboutthestrainonthestar'scrust.

TheeffectofGravitationalDistortionofSpacetimeonPulsarTiming

SatoruSakai (UniversityofGlasgow)withGraham Woan, and MartinA. Hendry

Theaimofthisresearchistodeterminetheimpactofgravitationallensingonpulsartiming, anditsimplicationsforthedetectionofgravitationalwaves. Gravitationallensingoccurswhenamassivebodypassesclosetotheline-of-sightbetweentheEarthandasource. FromGeneralRelativity, thiscausesspace-timedistortionswhichresultinanextrapathlengththatthelightmusttravel, andsubsequentlyadelayinthetimeofarrival. Thisresearchwilllookattherateofchangeof(gravitational)Shapirotimedelay.

IntermittentRadioEmissionfromPSR B0823+26NeilYoung (UniversityofManchester)with

M. Kramer, A. Lyne, B. Stappers, and P. Weltevrede

Intermittentpulsarsarecharacterisedbyperiods,uptoyears, whentheirradioemissionisofffollowedbysimilarlylongperiodswhentheyareon. Theyofferauniqueinsightintomagnetosphericphysicsofpulsars. PSR B0823+26isacandidateofthispulsarclass. IntensiveobservationsofthissourcewerecarriedoutwiththeLovellTelescope, atJodrellBank, fromJanuarytoJune2009. Thispulsarhassubsequentlybeenfoundtoexhibitquasi-periodicradioemissionphases, ontimescalesshorterthanthatobservedinthecanonicalintermittentpulsarB1931+24. Here,I presenttheresultsandanalysisoftheseobservations.

PulsarElectrodynamics: TheRelativisticKineticTheoryofRadiativePlasmas—TheGamma-ray

cut-offAntonioArmandodaCosta (InstitutoSuperior

Técnico, Lisboa, Portugal)with D.A. Diver,E.W. Laing, C.R. Stark, and L.F.A. Teodoro

Theclassicalmodellingofradiationbyacceleratedchargedparticlesinpulsarspredictsacut-offinphotonenergyataround25GeV.Whilstthisisbroadlyconsistentwithobservations, theclassicaltreatmentisnotself-consistent, andcannotbeextendedtoexplaintherarehigh-energydetectionsofphotonsinthe100sofGeV range. Inthispaperwerevisitthetheoreticalmodellingofhigh-energyradiationprocessesinverystrongelectromagneticfields, inthecontextofbothsingleparticlesandcollectiveplasmas, whichimpliesanextensionoftheVlasovtheoryofcollisionlessplasmas, totakeintoaccountradiativeprocesses. Therearenoclassicalconstraintsonthisdescription. Wefindthatthereisindeedacriticalenergyofaround50GeV thatarisesnaturallyinthisself-consistenttreatment,butratherthanbeingacut-off, thiscriticalenergysignalsatransitionfromradiationthatisclassicaltoaquasi-quantumdescription, inwhichtheparticleisabletoradiatealmostitstotalenergyinasingleevent. Thisnewmodellingthereforeplacespulsarradiationprocessesonamoresecurephysicalbasis, andadmitsthepossibilityoftheproductionofTeV photonsinaself-consistentway.

P31TheCo-EvolutionofMassiveGalaxiesandtheir

SupermassiveBlackHolesoverthelast11.5GyrsAsaBluck (UniversityofNottingham)with

Christopher Conselice, Omar Almaini, Elise Laird,Kirpal Nandra, and Mark Dickinson

Supermassiveblackholes(SMBHs)arenowthoughttobeaubiquitousconstituentofmassivegalaxies. Despitetheirrelativelysmallcontributiontothemassofgalaxies(< 1/1000)theyexertapowerfulinfluenceovertheirevolution–possiblytriggeringstarformationandbeingultimatelyresponsibleforshuttingthisstarformationoff. TightrelationshipsarefoundtoexistinthelocalUniversebetweenglobalpropertiesofhostgalaxies(suchasluminosity, stellarmassandvelocitydispersion)andthemassofthecentralSMBH.ThissuggestsacausalconnectionbetweengalaxiesandSMBHs, thenatureofwhichisstillpoorlyunderstood. I willintroducemyapproachtoinvestigatethiscausalconnectionthroughprobingtheredshiftevolutioninthe MBH - M∗relation. WeutilizeNIR imagingfromtheHSTGOODS NICMOS Survey(a180orbitHSTprogramtoimagetheGOODS fieldintheH band)andthePOWIR SurveyandcombinethistothedeepestavailableChandraX-raydata. Byconstructingavolumelimitedsampleof120activegalaxiesat z < 3, weconstrainthepossibleevolutionin MBH – M∗ tobelessthanafactorof2. Moreover, weuseEddingtonargumentstocalculatethetotalfractionofmassivegalaxiesthatwillundergoanactivephaseintheirevolutionsincez=3, findingthatgreaterthan25%ofallmassivegalaxieswillachieveX-rayluminositiesintheSeyfertregimeorbrighter. FromthiswededucethatthethetotalenergyreleasedbyAGNsincez=3isgreaterthan15timesthetotalbindingenergyofallmassivegalaxiesintheUniverse, withinthisredshiftrange. Thiscolossalreleaseofenergymusthaveprofoundimplications

82 P30–P31

ontheevolutionofgalaxies, withmanyramificationstilltobeproperlyunderstood.

Theimpactoffeedbackontheorbitalcontentofdarkmatterhaloes.

SarahBryan (UniversityofManchester)withScottT. Kay, and Shude Mao

Galaxiesarethoughttoformhierarchically,throughthemergingandaccretionofsmallersystems. Assuch, thereshouldbeobservationalsignaturesofthesemergingprocessesintheremnantgalaxy, providingdynamicalinformationaboutitsformationhistory. Weinvestigatetheorbitalcontentofdarkmatterhaloesinordertoexplorewhatobservationalsignaturesmayresult.Todothis, wehaveusedtheOverWhelminglyLargeSimulations, asetofstate-of-the-arthighresolutioncosmologicalhydrodynamicalsimulationsrunwithdifferentphysicalprescriptionsforthefeedbackprocesses. Wequantifytheeffectsofthefeedbackprescriptionsonthedynamicsandorbitsofthedarkmatterandstellarparticles, bycomparingrunswithnofeedback, withstellarfeedbackandwithfeedbackfromAGN.Wecompareresultsofspectralanalysisoftheorbitalcontentofthesesimulationsandquantifythechangeinfractionofboxorbitsasdifferentimplementationsoffeedbackareconsidered, illustratingtheinfluenceoffeedbackprocessesontheorbitalcontentofthehaloes. Wealsoinvestigatehowtheorbitalcontentofthesehaloesdependonseveralkeyparameterssuchastheirmass, redshiftanddynamicalstate.

Theorientationofaccretiondisksandjetsinquasars

EmilyDown (UK GeminiSupportGroup)withSteve Rawlings, Devinder Sivia, and Jo Baker

I willdescribehowtheorientationofasampleof19high-zquasarswasmeasuredby(i)fittingthebroadH-αlinewithamodelwhichincludestheemissionfromaflattened, extendedaccretiondisk; and(ii)bymodellingtheradiospectralenergydistributionwiththeassumptionthatthejetsareDoppler-boosted. Resultsare: (i)Theopeningangleoftheobscuringtorusisconsistentwithpredictionsoftherecedingtorusmodel; (ii)Apossiblez-dependentvelocityoffsetbetweenthenarrowlineregionandtheaccretiondiskisfound;(iii)Misalignedaccretiondisksandradiojets, apossiblesignatureofarecentgalaxymerger, arerare.

TheEnviromentsofAGN atz1JamesFalder (UniversityofHertfordshire)with

Jason Stevens, and Matt Jarvis

WepresentananalysisofalargesampleofAGNenvironmentsatz∼ 1 usingstackedSpitzerdataat3.6um. Thesamplecontainstype-1andtype-2AGN intheformofquasarsandradiogalaxies,andspansalargerangeinbothopticalandradioluminosity. Wefind, onaverage, that2to3massivegalaxiescontainingasubstantialevolvedstellarpopulationliewithina200-300kpcradiusoftheAGN,constituting a > 8σexcessrelativetothefield. Secondly, wefindevidencefortheenvironmentalsourcedensitytoincreasewiththeradioluminosityofAGN,butnotwithblack-holemass. ThisisshownfirstbydividingtheAGN intotheirclassicalAGN types, whereweseemoresignificantover-densitiesinthefieldsoftheradio-loudAGN.IfinsteadwedispensewiththeclassicalAGN definitions, wefindthatthesourceover-densityasafunctionofradioluminosityforallourAGN exhibitsapositivecorrelation. One

interpretationofthisresultisthattheMpc-scaleenvironmentisinsomewayinfluencingtheradioemissionthatweobservefromAGN.Thiscouldbeexplainedbytheconfinementofradiojetsindenseenvironmentsleadingtoenhancedradioemissionor, alternatively, maybelinkedtomorerapidblack-holespinbroughtonbygalaxymergers.

TheroleoffeedbackinMilkyWaysatellitegalaxyformationusinghighresolutionsimulations

SamGeen (OxfordAstrophysics)withAdrianne Slyz, and Julien Devriendt

Weusesub-parsecresolutionhydrodynamicsimulationsoftheMilkyWayathighredshifttoinvestigatetheformationoftheMilkyWaysatellitegalaxies. Weanalysetheinfluenceofsupernovafeedbackondwarfgalaxyformation, andtheefficiencyofreionisationinsuppressingstarformationinthesmallestgalaxies. Bylocatinggalaxiesinourhighredshiftsimulationandtrackingthemtoz=0usingahalomergertree, wecancompareourresultstopresent-dayobservationsandcommentonthehypothesisthatreionisationhaltsstarformationinthelowestmasshalos. Wealsoconsidertheeffectofaddinggasphysicstosimulationsoftheformationofdwarfdarkmatterhalos, andtheimpactthishasonthemissingsatelliteproblem.

ClusterandGalaxyEnvironmentsofQuasarsKathrynHarris (JeremiahHorrocksInstitute,

UCLan)with R.G. Clowes, I.K. Sochting,G.M. Williger, L. Haberzettl, L.E. Campusano, and

M.J. Graham

Usinggalaxyclustersandquasarsitispossibletolookatthelargescaleenvironmentofquasarsandthereforeinferwhichformationmechanisms(e.g.,mergers, hotgastheory, galaxyharassment)aremostlikelytooccur. Lookingatthisoverarangeofredshiftsandquasarluminositiesgivesanindicationofanyevolutionofthisrelationship.

UsingCanada-France-HawaiiTelescope(CFHT),CosmicEvolutionSurvey(COSMOS) andImamoriMagellanArealCameraandSpectrograph(IMACS)data, galaxyclusterredshifts, positions, andshapesweredetermined. Wherepossible, directionalinformationwasconservedinordertogivemoreenvironmentalinformation. Thisdatacoversanareaof4sq. degreesintotalandextendstoaredshiftof0.8fortheIMACS dataand1.3fortheCOSMOS data.

Preliminaryresultsshowthequasarsappeartoliepreferentiallyinadirectionperpendiculartothemajoraxisoftheclusterassociatedwithit. Thisdoesnotchangeovertheredshiftrange0.2-0.8.Preliminaryresultsalsosuggestthatathigherredshifts(z < 0.5)quasarsliefurtherawayfromtheclustersthanatlowerredshifts, withquasarsatredshiftslessthan0.25lyingonaveragebetweentwoandfourMpcfromtheclusterandforz > 0.5 theaverageisthreetosixMpc.Thesedistancesareproject2D distanceandtakenattheredshiftofthequasar.

DiskHeating: ComparingtheMilkyWaywithCosmologicalSimulations

ElisaHouse (JeremiahHorrocksInstitute, UCLan)with C.B. Brook, B.K. Gibson, P. Sanchez-

Blazquez, and S. Courty

Wepresenttheanalysisoffivesimulationsrunwithdifferentparticleandgrid-basedcosmologicalhydrodynamicalcodesandcomparethemwith

observationaldataoftheMilkyWay. Westudythevelocitydispersionversusagefordiskstarsatz=0andfindthatthreeofthesimulationsaremoreconsistentwithobservationsbyHolmbergetal.(2008)wherethestellardiskappearstoundergocontinual/secularheating. TheothertwosimulationsareinbetteragreementwiththeQuillen&Garnett(2001)observationsthatsuggesta``saturation"intheheatingprofileforyoungstarsinthedisk. Wealsoanalysethekinematicsofdiskstarsatthetimeoftheirbirthfordifferentepochsinthegalaxy'sevolutionandfindthatinsomesimulationsstarsareborncoldwithinthediskandheatduetoacombinationofphysicaland/ornumericalprocesses, whileothersimulationspossessstellarpopulationswhichpresentlittleornoheatingwithtime. TwoofthemodelswhichareinbetteragreementwithobservationsoftheMilkyWay'sstellardiskundergosignificantlylowerminor-merger/assemblyactivityafterthelastmajormerger, i.e. oncethediskhasformed. Allofthesimulationsaresignificantly'hotter'thantheMilkyWaydisk, aproblemlikelyrootedintheunderlyingtreatmentoftheheatingandcoolingoftheinterstellarmedium, andtheresolution-dependentdensitythresholdforstarformation.

TheMulti-facetedX-rayactivityofthecomplete3CRR AGN sampleatz<0.1

ElizabethMannering (UniversityofBristol)withM. Birkinshaw, D.M. Worrall, D.A. Evans,M. Hardcastle, R.P. Kraft, and E.S. Perlman

WepresentChandraimagesof9previouslyX-rayunobservedsourcestocompleteobservationsofthe3CRR low-redshiftradiogalaxysample. The36sourcesofthecompletesamplealsohaveexcellentmulti-wavelengthradiodataandhavebeenimagedwithSpitzer(3.5-160microns)andwithHST.ThesamplespanstheimportanttransitioninradioluminositiesandmorphologyfromFRI toFRII type. Theimagingandspectroscopyofthecores, jets, hotspotsandatmosphereswillbeofpermanentlegacyvalue.Thispostergivesafirstlookatthesedataandindicateshowweplantoinvestigateparticleaccelerationmechanisms, interactionsbetweenradioplasmaandtheISM andIGM,theemissionmechanismofhotspots, andAGN fuelling

MomentumdrivenfeedbackfromstellarnucleiRachaelMcQuillin (KeeleUniversity)

InthelastdecadeobservationswiththeHubbleSpaceTelescope(HST) haverevealedthepresenceofmassivestarclustersatthecentresofthemajorityoflowandintermediatemassgalaxies.Anunexpectedobservationalresultisthatnuclearclustermass, Mnc, scaleswiththevelocitydispersionofthehostgalaxybulge, σ. TheMnc − σ relationisanalogoustothatbetweenthemassesofcentralsupermassiveblackholes(SMBHs)andthevelocitydispersionsoftheirhostgalaxybulges. Theobserved M–σ relationcanbeunderstoodasaconsequenceofmomentumconservingfeedbackfromthenucleuswhichsweepstheambientmediumintoashellthatexpandsintothegalaxy. Thereisacriticalmassofthenucleusforwhichtheshellcanescapethegalaxyhencecuttingoffthegrowthofthenucleusandlockinginthe M–σ dependence. Previousworkhasmodelledthisprocessingalaxieswithsingularisothermaldark-matterhaloes. Inthiscontribution, weextendthisworkandinvestigatethe M–σ relationthatresultsfromnuclearfeedbackingalaxieswithmorerealisticdark-matterandgasdensityprofiles.

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TheColdGasContentofBulgelessDiskGalaxiesKatePilkington (JeremiahHorrocksInstitute,UCLan)with Brad Gibson, ChrisB. Brook,

Greg Stinson, and Francesco Calura

Wepresentananalysisoftheneutralhydrogen(HI) propertiesofasetoffullycosmologicalhydrodynamicaldwarfgalaxysimulations. AsreportedrecentlybyGovernatoetal. (2010), thesesimulationsarethefirstoftheirkindtoresultinthesuccessfulreproductionofa(dwarf)spiralgalaxy,withoutanyassociatedstellarbulge.  Inablindexperiment, wehavenowsetouttocompareindetailtheHI distributionandkinematicsofthesesimulatedbulgelessdiskswiththoseofthreecomparabledwarfsfromtheTHINGS (TheHINearbyGalaxySurvey)archive.  Wewishtoanswerthequestion"Arethegaspropertiesofthefirstsuccessfullysimulatedbulgelessdwarfsconsistentwithobservations?".  Todoso, wehavethusfarextractedfromthesimulations, radialandverticaldensityprofiles, scalelengths, andspatially-resolvedmapsofscaleheights(eg.flaring, warping)andvelocitydispersion(eg.velocityellipsoid, turbulence).  Ourhighestresolutiondwarfshowsseveraluniqueandchallengingcharacteristics(relativetotheTHINGSobservationsofcomparabledwarfs)whichweareinthemidstofquantifying, including(i)ahigh-densitycoldgascorewithintheinner1kpc(10timesthedensityatoneHI diskscalelength), (ii)significant, andcontinual, diskflaringfromtheinnertotheouterHI disk(factorof10increaseinscaleheightperdexincreaseinradius), and(iii)asignificantly(kinematically)colderHI disk(factorof5lowerlines-of-sightvelocitydispersions,relativetoHoII,NGC4214, andIC2574).  Wewilldiscusstheramificationsofourpreliminaryanalysesintermsofthedefiningrolesplayedbyenergyfeedbackandstarformationthresholdsinsuchcosmologicalhydrodynamicalsimulations.

SearchingforComptonThickAGN atz2indeepX-rayfields

CyprianRangel (ImperialCollegeLondon)withKirpal Nandra, Elise Laird, and James Aird

CurrentlytheX-rayemissionfromAGN failstofullyaccountfortheobservedX-rayBackground(XRB) atharderenergies. IthasbeentheorizedthisisduetoapopulationofobscuredAGN thatwehaveyettoobserve. ComptonThick(CT) AGNhaveobscuringgasofthesurroundingtoruswithNH > 1024 cm−2, thustheX-rayemissionfromthecentralsourceisheavilysuppressed. WepresenttheresultsofasearchforCT AGN atz∼ 2

indeepX-rayfields. WeidentifyX-raydetectedAGN throughLikelihoodRatio(LR) matchingofopticalandNIR photometrytoX-raydata.SometimesCT AGN aredetectedviascatteredorreflectedX-rayemissionfromthecentralsource,butatz∼ 2 suchtheseprocessesmaybetoofainttoyieldadetection. StackingisthereforeusedtotestforthepresenceofX-rayemissionfromcandidateCT sourcesselectedviatheirmulti-wavelengthproperties.

StellarFeedbackinSPH GalaxyFormationSimulations

GregStinson (JeremiahHorrocksInstitute, UCLan)with Chris Brook(UCLan), Jeremy Bailin(Michigan), Sarah Nicerkson(McMaster),

Hugh Couchman(McMaster), and James Wadsley(McMaster)

WepresentastudyofgalaxiesandtheiraccompanyingsatellitedwarfgalaxiesfoundintheMcMasterUnbiasedGalaxySimulations, aseries

of15cosmologicalSPH simulationsofMWmassedobjects. Inthesesimulationsthatformarangeofgalaxymorphologies, wefindthatthesatelliteluminosityfunctionsaresimilartowhatisfoundintheLocalGroupwheneffectivestellarfeedbackisutilized. Oneoftheproblemswiththegalaxiesformedinthesesimulationsisthedensecentralconcentrationofmatterfoundineverygalaxy. Weexplorepossiblesolutionstothisproblemusingalternatestarformationandstellarfeedbackrecipes.

Superstarclusterfeedbackfromlocaltogalaxyscales

MarkWestmoquette (UCL)

Understandingstarburst-drivenoutflowsisimportantformanyreasonswithinthecontextofgalaxyevolution. However, tounderstandoutflowsonthelargescale, thedetailsoffeedbackmechanismsfromindividualstarclustersmustfirstbeunderstood. I willdiscussrecentresultsfromanumberofhighspatialandspectralresolutionintegralfieldspectroscopicstudiesoftheionizedgasenvironmentwithinasampleofnearbystarbursts. Thesestudiesareallowingustobuildupapictureof(1)howpowerisfedfromsuperstarclustersintothesurroundingISM,(2)howtheISM propertiesaffecthowthispowerisdirected,and(3)howthegasoutflowsevolvestructurallyandenergeticallytowardsthelarger-scales.

StabilityandevolutionofclustergalaxiesinMOND

XufenWu (PhysicsandAstronomy, UniversityofStAndrews)with Hongsheng Zhao, Yougang Wang,

Benoit Famaey, and Martin Feix

FollowingSchwarzschild'sapproach, weconstructaseriesofHernquistmodelsembeddedinexternalfieldsintheframeworkofMOdifiedNewtonianDynamics(MOND).Thesemodelsrepresentmedium-massellipticalgalaxieswithmildcuspswithinagalaxycluster, providingaMONDianexternalfieldontheorderof gext ≈ a0. UsingN-bodysimulations, wefurthertestthestabilityofthesemodels. WefindthattheSchwarzschildmodelsarenotinrigorousequilibrium. Theoutskirtsofthegalaxiesdeveloplopsidedshapesalongtheexternalfield'sdirection, andtheradiicontaining 90%ofthetotalmassincreasebyafactorof 2 during 60 simulationtimes(NewtonianKepleriantimesatscalelengthof 1kpc)afterwhichthemodelsseemtosettletoastableequilibrium. Comparingourresultstoanisolatedgalaxymodel, theSchwarzschildmodelsinexternalfieldsarelessself-consistentandstable.

P32StellarmagnetismthroughtheeyesoftheFORS1

instrumentoftheESO VLTStefanoBagnulo (ArmaghObservatory)with

L. Fossati, C. Izzo, J.D. Landstreet, C. Folsom, andO. Kochukhov

Duringafulldecadeofoperations, theFORS1instrumentoftheESO VeryLargeTelescopehascollectedalargeamountofmagneticfieldmeasurementsofvariouskindsofstars. TogetherwiththeESPaDOnS instrumentoftheCanada-France-HawaiiTelescope, withtheMuSiCoS andNARVAL instrumentsofthe2mTelescopeBernardLyotofthePic-du-MidiObservatory,FORS1hasbeenoneoftheworkhorseinstruments

fortheobservationalstudiesofstellarmagnetism.Severalinterestingdetectionswereobtained, someofthemwereeventuallyconfirmedbyfollow-upinvestigations, somewerenot. Wehaveperformedahomogeneus(re-)analysisofthefullFORS dataarchive, andinthistalkwewillgiveanupdatedreviewoftheincidenceofthestellarmagnetisminvariousclassesofstars.

InvestigatingtheX-rayEmissionofA-typeStarsThroughtheMagneticActivityofUnresolved

LowerMassCompanionsRobertDeRosa (UniversityofExeter)with

J. Bulger, J. Patience, B. Leland, and B. Macintosh

WepresenttheresultsofaninvestigationintothesourceofX-rayemissionfromnearbyearly-typestars. ByutilisingtheROSAT All-SkySurvey(RASS) brightandfaintsourcecatalogues, andthepreliminaryresultsfromourongoingmultiplicitysurveyofA-typestars.

Bremsstahlungemissionhasbeendetectedfromnumerousmain-sequencestars, fromO-M.StudiesofmassivestarsshowX-rayluminosityscalingasafunctionofthestellar-winddensity, suggestingthatthesestrongradiativelydrivenwindsaretheprimarygeneratingmechanism. ForlessmassivestarstheX-raygenerationisthoughttobeduetoadynamoeffectcausedbydifferentialrotation. Starsfrommid-B tolate-A haveinsufficientluminositytodrivemassivewinds, norhavesufficientlydeepconvectiveenvelopesandshouldtheoreticallyhavelowX-rayemission. Contrarytothesepredictions, X-rayemissionhasbeendetectedfromnumerousnearbyA-typestars. Thedetectionoftwolow-massstellarcompanionstoX-rayemittingA-typestars(e.g. AlcorB) wouldsuggestanX-raygenerationmechanismfortheseanomalousstars- unresolvedcompanions.

WithinthisstudywehavecompiledadistancelimitedsampleofnearbyX-raydetectedA-typestars, alongsideacontrolsampleofnonX-raydetectedA-typestars. Thetypicalangularresolutionachievedinourobservationswas∼ 0.1"withthenarrowbandexposuresallowingustoresolve ∼ 10AU binaries, whilstsensitivitytothebottomofthemainsequencewasachievedat∼ 1 − 2"withthelongerbroadbandexposures.WefindthatagreaterproportionofX-raydetectedA-typestarshaveanassociatedcompanioncomparedwiththoseinthecontrolsample,suggestingthatunresolvedlow-masscompanionsareindeedasourceofA-starX-rayemission.

TestingtheabilityoffieldextrapolationmodelstopredicttheX-raypropertiesofpre-mainsequence

starsScottGregory (UniversityofExeter)with

E. Flaccomio, C. Argiroffi, J. Bouvier, J.-F. Donati,E.D. Feigelson, K.V. Getman, G.A.J. Hussain,M. Ibrahimov, M. Jardine, and F.M. Walter

Byextrapolatingfromobservationallyderivedmagneticsurfacemaps, obtainedthroughZeeman-Dopplerimaging, modelsofstellarmagnetospherescanbeconstructed. Byassumingthattheplasmatrappedalongtheclosedfieldlinesisinhydrostaticequilibrium, coronalX-rayemissionproperties, suchastheglobalX-rayemissionmeasureandtheamountofrotationalmodulationofX-rayemission, canbepredicted.Forpre-mainsequencemagnetospherestheanalysiscanbeextendedtoincorporateaccretionflows, andpredicttheamountofsofterX-rayemissionfromaccretionspotsthatwouldbeobserved. I willdetailthepreliminaryresultsofanambitiousmulti-wavelength, multi-observingsite,

84 P31–P32

andnearcontemporaneouscampaign, combiningspectroscopicoptical, nIR,UV,X-ray(200ks,Chandra), spectropolarimetricandphotometricmonitoringoftheaccretingpre-mainsequencestarV2129Oph. Surprisinglythenewmagneticmapderivedfromthe2009dataappearstoindicatethatthesurfacemagneticfieldhasundergonelittleevolutionsinceitwaspreviouslyobservedin2005. ThedatasetalsoallowsX-rayemissionfromthestellarcoronaandtheaccretionhotspotstobedisentangledandcruciallyallowsthevalidity, andthepredictions, ofthe3D fieldtopologiesderivedviafieldextrapolationtobecriticallyexamined.

Stellarmagnetisminsolar-typestarsGaiteeHussain (ESO)

Magneticfieldsplayaroleatalmostallevolutionarystagesoflowmass(F toM-type)stars.Onthepre-mainsequence, strongkG fieldschannelaccretionfromcircumstellardisksontothecentralT Tauristars; whileinolderplanet-hostingsystemswefindevidenceofmagnetosphericinteractionbetweenplanetsandtheirhoststars.

ZeemanDopplerimagingtechniquesenableustomapstellarsurfacemagneticfieldsinunprecedenteddetail. Magneticfieldmeasurementsmadefrommagnetically-sensitiveintensitylineprofilesfurthercomplementandenhancetheinformationgainedfromthesesurfacemagneticfieldmaps. Thelatestresultssuggestthatthesizeandcomplexityofsurfacemagneticfieldsdifferinfullyconvectivestarsandstarswithradiativecores. A furthertransitionoccursasstarsspindownovertime.

I willreviewourcurrentunderstandinganddemonstratehowmagnetosphericmodelsoflowmassstarsbasedonsurfacemagneticfieldmapsaretestedusingmulti-wavelengthobservations.Finally, I willgiveanoverviewoftherichfutureprospectsofthisfieldinlightofnewinstrumentsandfacilities, bothintheshortandlong-term.

MagneticactivityinfastrotatingM-dwarfsaboveandbelowthefullyconvectiveboundary

RobJeffries (KeeleUniversity)with Richard Jackson

WepresentresultsfromsurveysofcoronalandchromosphericactivityamongfastrotatingM-dwarfsbelongingtotheyoungopenclustersNGC2547andNGC 2516. OurtargetsarecoolclustermemberswithknownrotationperiodscoveringspectraltypesfromK3toM5. Coronalactivityappearstobecontinuousacrossthefullyconvectiveboundary, wherealmostallthefullyconvectivestarsexhibitsaturatedX-rayemission.However, thelevelofsaturatedchromosphericemissiondeclinesbyfactorsof2-3forstarsofspectraltypeM3andcooler, coincidingwithboththefullyconvectiveboundaryandadramaticincreaseinaveragerotationrates. Noevidencefor"supersaturation"wasfoundinthechromospheresorcoronaeoftheM-dwarfs. Wediscussthesefindingsintermsofchangingmagnetictopologies.

TheDopplerShadowofWASP-3bGrantMiller (UniversityofStAndrews)

Hot-jupiterplanetsforatlargedistancesfromtheirhoststarsthenmigrateinwardstotheirobservedorbitalseparations. Themechanismsresponsibleforthisarenotfullyunderstoodbutthespin-orbitalignmentofthesystemgivescluesastohowtheplanetsmigrated. Thespin-orbitalignmentcanbemeasuredbyanalysingtheRossiter-McLaughlin

effect. Thisistheradialvelocityanomalycausedbyaplanetasittransitsthestellardisc. WedescribeanewtomographicmethodforanalysingtheRossiter-McLaughlineffectandpresenttheresultsofitsapplicationtotheWASP-3system.Wealsoexplainhowthismethodcanbeusedtoconfirmtheexistenceofplanetsaroundearly-typestarspreviouslyinaccessibletoplanethuntersduetotheirrapidrotationandlackofspectrallines.

Theinfluenceofthestellarwindonclose-ingiantplanets

AlineVidotto (UniversityofStAndrews)withM. Opher, V. Jatenco-Pereira, and T.I. Gombosi

Sincethefirstdiscoveryofextrasolarplanets, morethan300planetshavebeendetected, manyofthemlocatedverynearthehoststar. Becauseofsuchextremeproximity, interactionoftheplanetwiththestarisexpectedtogiverisetoavarietyofphenomena. Thestellarwindisexpectedtodirectlyinfluencetheplanetanditsatmosphere,e.g., bychangingtheconfigurationoftheplanet'smagnetosphere, producingnonthermalplanetarymagnetosphericradioemissions, etc. Sofar, thefewtheoreticalworksinvestigatingtheinfluenceofthestellarwindonthemagnetosphereofplanetswerebasedonsimplifiedtreatmentsofthestellarwinds. Wedevelopedthree-dimensionalmagnetohydrodynamicsmodelsofstellarwindswhichenabledustodetermineself-consistentlythecharacteristicsoftheimpactingwindontheplanet. Underrealisticstellarwindconditions, weanalyzedtheinfluenceofthewindonplanetmigrationbyestimatingthemigrationtime-scaleduetodragforcesexertedbythestellarwindonahot-Jupiter. Furthermore, wealsoestimatedthepowerreleasedfromthemagneticinteraction(reconnection)betweenamagnetizedwindandthemagnetosphereofaclose-ingiantplanet. Weshowthatthecharacterizationofthewindpropertiesofthehoststarisessentialforadeeperunderstandingofextrasolarplanetarysystems.

P33Astronomyinthecurriculum. Developmentsat

KS4andKS5CharlesBarclay (MarlboroughCollegeandOxford

Astrophysics)

Educationisthefuture. Childreninfluenceparents('thepublic')andthencepoliticalperceptionofasubject'simportance. IfinherententhusiasmforAstronomyatages10and11canbemaintainedwiththepotentialofaqualificationatGCSE,IbelievepupilenthusiasmforSciencecanbeenhancedwiththeaddedbenefitthatthesubjectisequallyappealingtobothgirlsandboysatthislevel. TheGCSE inAstronomycontinuestogrowexponentiallyandthenewSpecification,developedwithschoolteachersandprofessionalastronomers, implementedin2009forfirstexamin2011, lookstoseeanotherhikeinpupilnumbers. AtKS5, thedevelopmentoftheExtendedProjectinitiativealsoallowsforin-depthpupilmotivatedstudyofastronomicaltopicsinthesixthform. I willoutlinethecurrentpositionanddiscussthepotentialofthesequalifications

TheBigBang!DanielleBewsher (JeremiahHorrocksInstitute,

UCLan)with D.S. Brown, J.M. Wild, L.M. Green,G.M.H. Wilkins, M. Marsh, C. Alexander, J. Kelly,S. Dalla, R.W. Walsh, H.E. Mason, and M. Popescu

The'BigBang'isanationalSTEM outreachactivitywhichstartedNationalScienceweekin2010. TheUniversityofCentralLancashireledacollaborationofsolarphysicistsfromaroundtheUK toproducethe'LivingwithaStar'exhibitionstandattheBigBang. Thispresentationwilldiscussthehighs/lowsandpitfallsoforganisingsuchevents!

OutreachduringInternationalHeliophysicalYearLucieGreen (UniversityCollegeLondon–MSSL)

2007to2009wasdesignatedasInternationalHeliophysicalYeartocelebrate50yearsofspacescienceandsolarsystemphysics. TheUK joinedinwithaseriesofeventswhichranacrossthecountry. Thistalkwillgiveanoverviewoftheactivitiesthattookplaceandlessonslearned.

DevelopmentofanAll-SkyCameraforOutreachActivities

MartinHendry (UniversityofGlasgow)withGiles Hammond

TheChargeCoupledDevices(CCD's)foundincommercialCCTV camerasofferhighsensitivityatlowcost. However, intheiroff-the-shelfformthesecamerasarelimitedtoamaximumexposureof1/5sbyanelectronicshutterandarethereforeoflittleuseforimagingdeepskyobjects. WithminormodificationstothecircuitboarditispossibletodisablethisshutterandcontroltheclockpulseswhichareusedtoreadouttheCCD.Thisallowsforlow-lightimagingofastronomicalobjects.

Overthepastcoupleofyearsanall-skycamerahasbeendevelopedattheAcreRoadObservatory,UniversityofGlasgow. ThisdevicecomprisesaCCTV surveillancecamerainaweatherproofboxwithanacrylicdome. A wideangle(1.6mmfocallength)lensisattachedtothefrontofthecameraandthisoffersanalmostfull180degreefieldofview. Byadjustingtheexposurelengththecameraisabletooperatebothindaylightandalsoduringthenight. Fromtheurbanlocationoftheobservatorythisallowsobservationofbrightstarsandthemoon/planetstogetherwithobservationofcloudstructuresandotherinterestingmeteorologicaleffects.

Thecaptureprogram(developedinMATLAB) iscapableofrunningonanyWindowsXP machine(connectedtotheinternet)andautomaticallyselectsthecorrectexposure/savestheresultingimageasaJPEG.Theseimagescanthenbecombinedintoamoviefortheday. A secondcameraisnearingcompletionanditwouldbeidealifaschool/astronomicalsocietywithadarkskylocationwouldbewillingtohostthisdevice.Theimagesfromthecameracouldbeuploadedtotheinternetandwouldbeanexcellentoutreachandlearningtool.

TheScottishSolarSystemMartinHendry (UniversityofGlasgow)

AspartofaScotland-wideprogrammeofpublicoutreachforIYA2009, the"ScottishSolarSystem"projectwasapartnershipbetweenGlasgowUniversity, GlasgowScienceCentreand14Scottishastronomyclubsandsocieties. Theprojectcoordinatedarangepubliceventsacross

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thecountry, heldatlocationswhich- withGlasgowScienceCentreastheSun- duringAutumnMoonwatchweekcreatedascalemodeloftheSolarSystem, withcorrectlyscaledphysicalobjectsateachoftheplanetarylocations.

InthistalkI willbrieflyreviewthesuccessesoftheScottishSolarSystemproject, andconsideritslegacyforfutureastronomyoutreacheventsinScotlandandbeyond.

IYA 2009ontheBigIslandofHawaiiIngeHeyer (JointAstronomyCentre)with

Janice Harvey(GeminiObservatory),Peter Michaud(GeminiObservatory),KumikoS. Usuda(SubaruTelescope),

Gary Fujihara(UniversityofHawaiiatHiloInstituteforAstronomy), and Shawn Laatsch

(`ImiloaAstronomyCenterofHawaii)

TheInternationalYearofAstronomy(IYA) 2009combinedtheoutreacheffortsofalltheobservatoriesonMaunaKea, whichincludestheUnitedKingdomInfraredTelescope, theJamesClerkMaxwellTelescopeandtheGeminiNorthObservatory. IYA allowedtheMaunaKeaObservatoriesOutreachCommittee(MKOOC) tobrandourannuallocaleventswhiledevelopingseveraluniqueandinnovativeactivitiesandproducts. OurflagshipJourneythroughtheUniverse(JTTU) programmeintroducedtheGalileoscope. JTTU’steachertrainingprogrammesandfamilyscienceeventswereenhancedwithIYA cornerstoneactivities. Bycollaboratingwithourlocalnewspaper, 70,000copieswerepublishedofaspecialtabloid“StarsOverMaunaKea”. OurgroupadditionallycontractedawebsiteonIYA onthelocalnewspaper’swebsitewhichin2009receivedover1.7millionhits, andwhichhasbeencontinuedforthisyear. AstronomytradingcardswereproducedforourlocalAstroDayandtheGalileoBlockParty, thelatterbeingoureventfortheGalileanNightsinvitingtheentirelocalcommunitytotheobservatoryfacilities. A postercontestencouragedlocalstudentstocombineastronomyandtheirculturalbackgroundinauniqueartisticexpression. A year-longfreecollege-levelintroductoryastronomyclassgavelocalteachersastronomycontentandteachingtoolsfortheirclassroomsatallgradelevels. Thedirectorsofallobservatoriesgavemonthlypublicpresentationsintwolocationsonourisland, andtheMaunaKeaObservatoriesleadoffthe80-Telescopes24-hourwebcast. Photosandactivitiesfromalleventshavebeenarchivedonourwebsitestosharewiththeworld.

UK DarkSkyDiscoveryDanHillier (RoyalObservatoryEdinburghVisitor

Centre)

TheDarkSkyScotlandprogrammehasbeenrunningforthreeyearsinvolvingresearchastronomers, astronomystudents, amateurastronomersandsciencecommunicatorsinmorethan60publiceventsatlocationsthroughoutScotland. IthasestablishedDarkSkyDiscoverySitesinlocalcommunitiesandaStargazersWelcomeschemefortourismbusinesses. UK DarkSkyDiscovery, 2010-2012, aimstorunsimilarprogrammesthroughouttheUK basedonsimilarpartnershipsinWales, NorthernIrelandandtheEnglishregions.

Beyondconstellationstories: communicatingcutting-edgescienceandengagingnewaudiencesthroughnovelplanetariumprogrammingforthe

InternationalYearofAstronomyOliviaJohnson (RoyalObservatoryGreenwich)

with Claire Bretherton(CarterObservatory), andMarek Kukula(ROG)

Ofthe1.4millionvisitorsattractedbythewiderangeofexhibits, events, talks, andworkshopsattheRoyalObservatoryGreenwich(ROG) duringtheInternationalYearofAstronomy(IYA),over130,000attendedaplanetariumshowatthePeterHarrisonPlanetarium(PHP).OpenedinMay2007, thePHP isnowtheonlyplanetariuminLondonandusestheprogrammableDigistar3systemtodeliveracombinationofliveandpre-recordedshowstoschoolandpublicaudiences.

DuringIYA,theScienceEducationteamattheROG explorednewwaysofexploitingtheintrinsicexcitementandsenseofconnectionwiththenightskyofferedbyimmersiveplanetariumshowstosupportandenhancethebroadrangeofsciencecommunicationeffortsacrosstheObservatory.Wewereparticularlyinterestedinmovingbeyondconstellation-basedtoursofthenightskytocommunicateup-to-the-minuteastronomicaldiscoveriesandengagenon-traditionalaudienceswithinthedome.

Inthistalk, I'llreportonavarietyofnewplanetariumcontentproducedattheROG duringIYA,including"VisionsofSaturn", developedincollaborationwiththeCassini-Huygensteamtoconveytheexcitementoftheirongoingresearchtofamilyaudiences, and"Sci-FiUniverse",developedincollaborationwiththeSci-FiLondonFilmFestivaltoengagefilm-goingaudiencesinthesciencebehindsciencefiction. Lookingtothefuture, I'llaskhowinnovativecollaborationwithplanetariacouldbenefitsciencecommunicationintheUK beyondIYA.

SongsoftheStars: theRealMusicoftheSpheresDonaldKurtz (JeremiahHorrocksInstitute, UCLan)

with R. Jain, M. Thompson, M. Roth, R. New,Y. Elsworth, W. Chaplin, I. Roxburgh, and

D. Gough

TheRoyalSocietySummerScienceExhibitionin2010willbeheldintheSouthbankCentreinLondonfor9daysfrom26Juneto4JulyincelebrationoftheRoyalSociety’s350thanniversary. Wewillhaveanexhibit, “SongsoftheStars: theRealMusicoftheSpheres”, thatwillbeabouthelioseismologyandasteroseismology.Aspartofouroutreachplanswehavemadetwoposters-- onegeneralforhomedisplay, andtheothermoredetailedforclassroomuse- thatwewillgiveawayas“freebies”tothousandsofthe30,000peopleexpectedtoattendtheexhibition.Our“poster”hereatNAM isthedisplayofthesetwofreebieposters, withsomecopiesavailableforyoutotakeaway, shouldyouwishtodoso. TheproductionofthepostershasbeensupportedbytheHelio- andAsteroseismologyNetwork(HELAS),aCoordinatedActionfundedbytheFP6-Infrastructure-ProgrammeoftheEuropeanCommission.

4YearsofPodcastingStuartLowe (TheJodcast)with JodcastTeam

Since2006wehavebeenproducingaregularpodcastcoveringastronomyandspacescience.Wereportasummaryofourexperiencesoverthepastfouryearsincludingourlistener/viewing

figures, feedbackandadescriptionofourliveepisoderecordedinlate2009.

SchoolsoutreachfortheGlasgowNAMAlecMacKinnon (UniversityofGlasgow)

PriortoNAM,pupilsinseveralschoolsaroundthegreaterGlasgowareahavebeenworkingonalittleresearchproject, findingoutalltheycanaboutsunspotsandforminganopinionontheroleofsolaractivityinclimatechange. Theywillpresentposterssummarisingtheirfindingsatasessiontoday. Wedescribehowandwhythisprojectwassetupandgiveatrailerforthepostersession.

Sun|trek- thefinalfrontierHelenMason (UniversityofCambridge)with

Sun|trekteam

Sun|trek(www.suntrek.org)isawebsiteabouttheSunanditseffectontheEarth. Itisaimedatschoolchildren. Itisgrowingfromstrengthtostrength, withover14,000userspermonthworldwide. Itisnowlinkedtomanywebsites(NASA,RAS,IoP,schoolscienceandtheBBC).WehavesomefundsfromSTFC toupdateSun|trekandwouldlikesomehelpandideasfromouryoungersolarresearchers. Findoutmore...

TheMusicoftheSunasaStarRichardMorton (UniversityofSheffield)with

R. Erdélyi

TheSun, atypicallate-typestar, isahighlydynamicplasmathreadedbyarathercomplexandubiquitousmagneticfield. Thismagneticfieldprovidesthefoundationsforawidevarietyofplasmastructureinthesolaratmosphere. Amongsuchstructuresaree.g. coronalloops(huge, oftenhundredsofMmlongmagneticloops), coronalholes(openmagneticstructures)orprominences(eruptivemagneticstructures, frequentlycausingdisruptionsinspaceweatherconditions). Becauseoftheirelasticnature, eachofthesemagneticfeaturesinthesolaratmospherecansupportanarrayofmagneto-hydrodynamic(MHD) oscillatorymodes. Fromaphysicalpointofview, therearetwofundamentallydistinguishabletypesofoscillatorymodesthatattractattention.Transversaloscillationsofcoronalloops, drivenexternallybyeruptivesolarflares, whichcanbethoughtofanalogoustosomeonepluckingaguitarstring. Ontheotherhand, therearelongitudinaloscillationsofmagneticloops, driveninternallybynano/micro-flares, whicharesimilartosomeoneblowingawindinstrument. Inthissense, theubiquitousmagneticoscillationsofthesolaratmospherearethemusicoftheSun!

Theoscillatorymodesofmagneticstructuresaredeterminedbytheinternalphysicalparametersofthesestructures(e.g., strengthofmagneticfield,temperature, density). ObservingtheMHDoscillationsprovidesauniqueandunprecedentedmethodforobtainingcrucialinformationabouttheotherwisedirectlyunobservable, internalpropertiesofsolaratmosphericplasma. Thistechnique, calledsolarmagneto-seismologyorcoronalseismology, isanalogoustothetraditionalseismologyoftheEarthwherefromdetectingearthquakesattheEarth'ssurface, geologistsderivetheinternalsub-crustpropertiesofEarth.

Magneto-seismologyisarapidlyemergingfieldofsolarandspacephysicsprovingunprecedentedinsightintosolarandstellarmagneticstructures.Themethodreliesonthecomparisonoftheoreticallyderivedpredictionstoobservations

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andapplyingtheobservationstodeterminetheotherwiseunmeasurable, localplasmaparameters,e.g. themuch-sought-aftermagneticfieldanditsfinestructureinthesolarcorona. Understandingaccuratelytheplasmapropertiesinthesolaratmosphereisvitalforthepredictionofspaceweatherevents, whichhaveadirectimpactonmannedspacemissions, lifehereonEarthandmaintainingpowergridsandsatellites.

BeyondIYA2009: SustainableScienceEngagement

SteveOwens (IYA2009)

FollowingthesuccessofIYA2009, agreatdealofmomentumandexpertiseinpublicengagementhasbeendevelopedamongsttheastronomycommunityintheUK.

Howmightthismomentumbesustained, andwhatisnextforUK astronomyoutreach?

SteveOwens, UK Co-ordinatorforIYA2009

TheSocietyforPopularAstronomy'sTelescopesforSchoolsProject

HelenWalker (STFC RutherfordAppletonLab)

TheSPA startedplanningfortheInternationalYearofAstronomy(IYA2009)inApril2007, anddecidedtheywouldtryandsend1000telescopesto1000secondaryschoolsintheUK.Theprojectprovedtobeagreatsuccessandaroundone-quarterofUK secondaryschoolsnowpossessa70mmrefractingtelescopewithsupportmaterials.Workingwithteachers, aDVD wasprofessionallyproducedwithinstructionsonhowtosetupandusethetelescope, alessonplan, interviewsandadditionalinformation. STFC fundedthepurchaseofthetelescopesandtheRAS fundedtheproductionoftheDVD.TheSPA providedanewareaontheirwebsitetosupportthethreemoonwatchperiodswhenschoolswereencouragedtousethetelescopes, andSPAvolunteerslookedaftertheproject. Over85%oftheschoolswhorespondedtoasurveyattheendoftheyearsaidthetelescopewasavaluableadditiontotheirschoolsresources. Aroundtwo-thirdsoftheschoolshaduseditmorethanfivetimes, andtherewereover200entriesinthecompetitionforMoon-relatedartwork. Itisestimatedthatmaybe25,000to50,000childrenhavelookedthroughoneofthetelescopesduringIYA2009.

ChallengesofPublicEngagementwithChildreninCare

AlisonWallace (UniversityCollegeLondon–MSSL)

Childreninpubliccareareyoungpeoplewhoareinthecareoflocalauthoritiesorwhoarelookedafterbyfostercarersorinchildren'shomes. Thesechildrenaremorelikelytofallbehindatschoolwithonly13%ofattainingfivegoodGCSEscomparedwith62%ofallchildren. Theyalsohaveamuchhigherstatisticalchanceofbecomingunemployedwhentheyleaveschool. Therearearound60,000childreninpubliccareintheUK atanyonetimeandweexaminethechallengesfacedbythespacesciencecommunitytoengagewiththem. Wediscussthereasonsthatchildrenincarearelesslikelytoachievetheirpotentialandthefactorsthatshouldbetakenintoaccountwhenorganisingactivitiesforthem. WeinvestigateongoingschemesincludingtheLetterboxclubandlookatthefuturedirectionofoutreachactivitiesincludinganoutlineofaproposedprojectatUCL-MSSL.

DidtheSunEarthPlanworkout?JimWild (LancasterUniversity)with

sunearthplan.netteam

sunearthplan.netisaSTFC-fundedpublic-facingoutreachprojectdesignedtoinformthegeneralpublicoftheimportanceofsolarsystemresearchandhighlighttheUK'sleadingroleinthisfield. Inordertoachievethisaim, theprojecthasbroughttogetherresearchscientists, professionalweb-designersandpublishedsciencewriters.LaunchedinFebruary2007, tocoincidewiththelaunchoftheInternationalHeliophysicalYear, thesitehasattractedover400,000uniquevisits(withmonthlyvisitspeakingatnearly20,000)andinterestfromboththeonlineandtraditionalmedia. Visitorfeedbackindicatesthatthemajorityofvisitorsarewithinthetargetaudience- adultmembersofthegeneralpublicunconnectedwithscienceorteaching, roughlyhalfofwhichwerepreviouslyunawareofUK activitiesinspaceresearch. Assuch, sunearthplan.netisasuccessfulandcost-effectiveexampleofanonlinescienceandtechnologyoutreachproject. Inthispresentationwehighlighttheproject'ssuccesses,reflectonthegreatestchallengesandsummarisethelessonslearnedthatmightbeappliedtootherprojectsinthefuture.

P34Magneticfluxemergenceandcoronaleruptions

intheSunVasilisArchontis (UniversityofStAndrews)with

AlanW Hood

Oneofthemostimportantprocesses, responsibleformanydynamicalphenomenaobservedintheSun, istheemergenceofmagneticfluxfromthesolarinteriorinactiveregionsandthemodificationofthecoronalmagneticfieldinresponsetotheemergence.

Inthistalk, wepresentnewresultsfrom3DnumericalMHD models, whichhavebeenusedtostudytheprocessofmagneticfluxemergenceintosuccessiveatmosphericlayers. WediscusstherecentprogressandtheconnectionbetweenfluxemergenceandpossibleinitiationmechanismsoferuptiveeventsintheSun.

Medium- andsmall-scaletransientsinthesolarwind

MarioBisi (AberystwythUniversity)withA.R. Breen, G.D. Dorrian, J.A. Davies, and

R.A. Fallows

Co-ordinatedobservationsofwhite-lightscatteringfromthesolarwindmadebytheSTEREOheliosphericimagers(HIs)andinterplanetaryscintillation(IPS) fromtheEISCAT facilityinMay2007revealedthepresenceofsignificantsmall-andmedium-scalestructure(onscalesoftensofthousandstohundredsofthousandsofkilometers)movingatspeedscomparabletothatoftheslowsolarwind. Thesestructureswereassociatedwithsignificantmagneticfieldrotationintheinterplanetarymedium, andappeartobeclosedorquasi-closedloop-likefeatures. Wediscusstheseobservationsintermsofthelighttheycastonslowwindstructure, andpresentawidersetofslowwindobservationswhereweinvestigatethepresenceofsmall- andmedium-scaleirregularitiesasacomponentofslowwindoutflow.

AnomalousSolarCyclesandtheEvolutionofCoronalHoles

BarbaraBromage (JeremiahHorrocksInstitute,UCLan)with Steven Chapman

A summaryoftheanomalousbehaviourofsolarcycle23iscomparedwiththatofthe15-yearcycle(cycle4)attheendofthe18thcentury. Ameansolarcycleisderivedandusedtocomparethecharacteristicsofthiscyclewithcycle23. Forexample, bothexhibittimeswhentheirevolutiondepartsfromthatofthemeancyclefor2or3years; priortothat, bothappeartoexhibitaphaseshiftofabouthalfasolarcycleinadvanceofaregular11-yearcycle(beginningwithzeroshiftatcycle1). SOHO-CDS synopticdatahavebeenusedtostudytheevolutionofcoronalholesthroughoutcycle23, atthesametimederivingthevariationintotalopenflux. In1998, thetwohemispheresdevelopedalagofabout2years,whichcanbeseentoleadtoadelayinthestartofthenextsunspotcycle, resultinginanextendedsolarminimum. Aswellaspredictingthenew-cyclestart, thedatasuggestthatcycle24willbeweak, lastinglongerthanthetypical11years.

ChiantiPy- A PythonInterfacetoCHIANTIKenDere (GeorgeMasonUniversity)

Pythonisafree, modern, object-orientedprogramminglanguagethatiswellsuitedtoscientificdataanalysis. A commandlineversionforusewithinaPythonshellisunderdevelopmentandwillbereleasedinthenearfuture.Programmatically, eachionintheCHIANTIdatabaseistreatedasanobject, providingagoodmatchtothestructureoftheCHIANTI database.ForanyionintheCHIANTI database, ChiantiPyisabletocalculateandplotlevelpopulations,spectrallineemissivities, contributionfunctions,G(n, T ), free-freeandfree-boundcontinua, andlineintensityratiosasfunctionsoftemperatureandelectronandprotondensity.

A pre-releaseversioncanbefoundathttp://sourceforge.net/projects/chiantipyandthecurrentdocumentationathttp://chiantipy.sourceforge.net.

RapidOscillationsintheSolarAtmosphereGarethDorrian (Queen'sUniversityofBelfast)with D.B. Jess, M. Mathioudakis, D.J. Christian,

F.P. Keenan, R.S.I. Ryans, and P.J. Crockett

RapidOscillationsintheSolarAtmosphere(ROSA) isahigh-cadence, highresolutionimagingsystemforstudyingthedynamicsolaratmosphere.ROSA consistsofsixcameraswhichcanbetunedtoobserveatdifferentwavebandsextendingfromthenearinfra-redtothenearultra-violet. Thiscapabilityenableshigh-cadencecharacterisationofsolaratmosphericphenomenaatmanywavebandssimultaneously. TheROSA camerascantakeupto30framespersecondinfullchipmodeorupto200framespersecondinwindowedchipmode. AttachedtotheDunnSolarTelescopeatSacramentoPeak, NewMexico;ROSA isnowavailableasanopenuserinstrumentfortheUK solarphysicscommunity. Thisposterpresentsasummaryoftheinstrumentcapabiltiesandsomeearlyresultsfromobservingcampaigns.Amongtheearlyresultsarehigh-cadencemulti-wavebandobservationsofintergranularmagneticbrightpoints, activeregions, sunspots, andlimbobservationsofsolarprominencesandspicules.

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Largeamplitudetransverseoscillationsinamulti-strandedEUV prominence, triggeredbytransient

disturbancesJenniferHarris (UniversityofWarwick)with

C. Foullon, V.M. Nakariakov, and E. Verwichte

WepresenttheanalysisoftwosuccessivetrainsoflargeamplitudetransverseoscillationsinanEUVprominence, observedontheNorth-Eastlimbon30July2005. Theoscillatorytrainsaretriggeredbytransientdisturbancesproducedbytwosuccessiveflares, whichoccurredabout10hoursapartinthesameremoteactiveregion(locatedjustnorthoftheequator, around500Mmfromtheprominence). WeusetheSOHO/EIT 195 Aimageswitha12minutecadencetocompareoscillatorypropertiesspatially, indifferentstrandsoftheprominence, andbetweenthetwosuccessivelyexcitedoscillatorytrains. Theevolutionoftheprominence'sapparentheightabovethelimbisdeterminedusing304/195 AimageratiosfromSOHO/EIT,andthiscorrectionisappliedtoaccountforthesolarrotation. Thevariousfilamentarystrandsareseentoexhibitdifferentoscillatorybehaviour, intermsoftheiramplitudes,phasesandperiods. Thelargestamplitudes, whichoccurattheprominenceapex, areover20km/sforthefirstoscillatorytrainandaround5km/sforthesecond, whiletheperiodatthislocationisapproximately90minutesinbothcases. Somestrandsshowdecayingoscillationswithadecaytimeofabout6hours, whileoscillationsofotherstrandsaredecaylessandlastforsevencycles. Wediscusshowtheobservationsmayshedlightonthenatureoftheoscillationsandthetriggeringmechanism.

TheMagneticPropertiesofFlaringActiveRegionsPaulHiggins (TrinityCollegeDublin)with

PeterT. Gallagher, D. ShaunBloomfield, andR.T. JamesMcAteer

TheSolarMonitorActiveRegionTracking(SMART)algorithmisanautomatedsystemfordetecting,tracking, andcatalogingmagneticfeaturesthroughouttheirevolutionanddecay. TheSMARTmethodwillformthebasisofactiveregionextractionandtrackingwithintheHeliophysicsIntegratedObservatory(HELIO).Magneticpropertiessuchastotalflux, fluximbalance, fluxemergencerate, Schrijver'sR-value, R*(amodifiedversionofR),andFalconer'smeasurementofnon-potentialityaredeterminedforindividualfeaturesthroughoutsolarcycle23.SolarflaresmeasuredbytheGOES andHSIinstrumentsareassociatedwithdetectedfeatures,andtherelationshipbetweenflaresizeandmagneticpropertyvalueispresented.

HardX-RayStructureofLoopFootpointsinaSolarLimbFlare

EduardKontar (UniversityofGlasgow)withNatasha Jeffrey, Iain Hannah, and Marina Battaglia

Weapplynewly-developedX-rayvisibilityforwardfittingtechniquetoRHESSI dataofawell-observedlimbflaretoinvestigatetheenergyandheightdependenceonsizes, shapes, andpositionofhardX-rayfootpointsources. Thepositions, theverticalextentsandthewidthsofhardX-raysourcesaremeasuredasafunctionofenergy. Ourobservationssuggestthattheverticalandhorizontalsizesoffootpointsaredecreasingwithenergywhilehigherenergyemissionoriginatesprogressivelydeeperinthechromosphere. ThecharacteristicwidthsofthehardX-rayfootpointsourcealongthelimbdecreasewithheightandareconsistentwithaconvergingmagneticfieldin

thefootpoint. TheverticalsizesofX-raysourcesarelargerthanpredictedbycollisionalthick-targettransportinasingledensityscaleheightchromospherebutcanbeexplainedusingamulti-threadeddensitystructureoftheloop.

NewsolarprominencediagnosticswithEIS/Hinode

NicolasLabrosse (UniversityofGlasgow)withB. Schmieder, and P. Heinzel

ObservationsofasolarprominenceobtainedwiththeExtremeUltravioletImagingSpectrometer(EIS)onHinodeareanalysed. TheobserveddecreaseinbrightnessofEUV coronallinescanbeduetotwobasicmechanisms: absorptionandemissivityblocking. TheabsorptionofcoronallineradiationinEUV isduetothephotoionisationofhydrogen,neutralandionizedhelium. Thesecondmechanismisthevolumeblocking, duetothepresenceofcoolplasma, oroflowdensityhotplasma(cavity). WeillustratethesemechanismsusingseveralEIS spectralwindows, andconcentrateontherasterat256A whichcontainstheHeII lineblendedwiththreeothercoronallines. Wepresentatechniquetoremovetheblendbetweentheselines, takingintoaccounttheabsorptionandemissivityblockingofthecoronallines, toretrievethetrueHeII lineprofileinordertomakeadiagnosticoftheplasmaindifferentpartsoftheprominence.

KineticAlfvénwavesandprotonvelocitydistributioninthesolarwind

XingLi (AberystwythUniversity)

Observationsofthesolarwindhaveshownthatprotonvelocitydistributionfunctionshavedistinctiveshapes: inthefastsolarwindtheprotontemperatureinthedirectionperpendiculartothebackgroundinterplanetarymagneticfieldishigherthanintheparalleldirection. Thissuggeststhatacontinuousheatingmechanismisneeded. ThecurrentunderstandingofincompressibleMHDturbulenceincreasinglypointstotheimportanceofkineticAlfvénwaves. Astheenergyatlargescalesisconvertedtosmallerscales, MHDturbulencetheorydictatesthattheturbulentwavenumberwillincreaseintheperpendiculardirectionwhiletheparallelwavenumberislargelyunchanged. WeinvestigatetheeffectofkineticAlfvénwavesonthevelocitydistributionfunctionsofprotonsinthesolarwind. FirstweuselinearVlasovtheorytoobtainthepropertyofkineticAlfvénwaves. Thesewavespropagateinthedirectionalmostperpendiculartothebackgroundmagneticfield. Wethennumericallysimulatehowthesewaveswillheatprotonsandshapetheprotonvelocitydistributionfunctions. Atalmostperpendiculardirection, wavesareusuallyregardedasnearelectrostatic. However, wewillshowthatthemagneticfieldofthesewavescannotbeneglected.

Simulationsofmagneticfluxemergencewithanoverlyingfield

DavidMacTaggart (StAndrews)with A.W. Hood

MHD simulationsoffluxemergenceallowonetomodelthelarge-scalestructureofthedynamicevolutionofactiveregions. Modelsthatincludeanoverlyingmagneticfield, fortheemergingfieldtointeractwith, allowforthepossibilityofinterestingphenomena, suchasCME initiation. Inthistalkwewillconsidersomeoftheseeffectsanddiscusstheirimplications.

Phasemixingofnon-linearAlfvénwavesJamesMcLaughlin (NorthumbriaUniversity)with

I. DeMoortel, and A.W. Hood

Weconsiderthebehaviourofnon-linear, non-idealAlfvénwavepropagationwithinaninhomogeneousenvironmentinboth1D and2Dandfindclearevidencefortheponderomotiveeffectandvisco-resistiveheating. TheponderomotiveeffectgeneratesalongitudinalcomponenttothetransverseAlfvénwave–withafrequencytwicethatofthedrivingfrequency.Analyticalworkshowstheadditionofresistiveheating. Thisleadstoasubstantialincreaseinthelocaltemperatureandthusthermalpressureoftheplasma, resultinginmaterialbeingpushedalongthemagneticfield. ConsideringAlfvénwavepropagationin2D withaninhomogeneousdensitygradient, wefindthattheequilibriumdensityprofileissignificantlymodifiedbyboththeflowofdensityduetovisco-resistiveheatingandthenon-linearresponsetothelocalisedheatingthroughphasemixing.

SDO/AIA responsetocoronalhole, quietsun,activeregionandflareplasma

BrendanO'Dwyer (UniversityofCambridge)withHelen Mason, and GiulioDel Zanna

WeexaminethecontributionofspectrallinesandcontinuumemissiontothechannelsoftheAtmosphericImagingAssembly(AIA) ontheSolarDynamicsObservatory(SDO) indifferentregionsofthesolarcorona. Syntheticspectrawereobtainedusingsampledifferentialemissionmeasures(DEM) forcoronalhole, quietsun, activeregionandflareplasma. Thesesyntheticspectrawereconvolvedwiththeeffectiveareaofeachchannel, inordertodeterminethedominatecontributionindifferentregionsofthesolarcorona. WehighlightthecontributionofparticularspectrallineswhichundercertainconditionscandramaticallyaffecttheinterpretationofSDO/AIAdata.

Alfvénwavephase-mixinganddampingintheioncyclotronrangeoffrequencies

JamesThrelfall (UniversityofStAndrews)withI. DeMoortel, and K.G. McClements

ThephasemixingofshearAlfvénwaveshasbeenproposedasamechanismforsolarcoronalheating[1]andsuchwavesmayalsoplayanimportantroleinflareheatingandparticleacceleration[2].Anytreatmentofshear-AlfvénwaveswithfrequenciesthatareasignificantfractionoftheiongyrofrequencymusttakeintoaccounttheHallterminthegeneralisedOhm'slaw. Weuseanumericalscheme, Lare2D,toinvestigatehowthephase-mixinganddampingofashear-AlfvénwaveareaffectedbytheinclusionoftheHallterm,whichsplitsitintoaleft-circularlypolarisedioncyclotronwaveandaright-circularlypolarisedwhistlerwave. Thepresenceofatransversegradientinwavepropagationspeedcauseswavedampingtooccurviaphase-mixing(HeyvaertsandPriest[1]), whichcanbeaffectedbythedispersivepropertiesoftheioncyclotronandwhistlerwaves.RunningLare2D forthecaseofasinglesmallamplitudeperturbation, wehaverecoveredresultsobtainedbyHoodet. al. [3]intheMHD limit.WearenowusingthecodetomodelthedampingofsuchapulseintheHall-MHD regime, andinthepresenceofequilibriumgradients.

ThisworkwasfundedbytheEngineeringandPhysicalSciencesResearchCouncil, throughaCASE awardandgrantEP/G003955, andbythe

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EuropeanCommunities, underthecontractofAssociationbetweenEURATOM andCCFE.TheviewsandopinionsexpressedhereindonotnecessarilyreflectthoseoftheEuropeanCommission.

[1]Heyvaerts, J.andPriest, E.R., Astron.Astrophys. 117, 220(1983)[2]McClements, K.G.andFletcher, L., Astrophys. J.693, 1494(2009)[3]Hood, A.W., Brooks, S.J., andWright, A.N.,Proc. R.Soc. Lond. A,458, 2307(2002)

AutomateddetectionandtrackingofmagneticfragmentsindecayingsolaractiveregionsFraserWatson (UniversityofGlasgow)with

Lyndsay Fletcher

Thebreakupanddecayofsolaractiveregionsisaprocessthatiscurrentlynotwellunderstood. Toprovidemoreinsightintothenatureofthedecay,wehavedevisedamethodforautomaticallydetectingmagneticfragmentswithinactiveregionsandtrackingthemthroughmultipleimages. Thisisdoneusing96minutemagnetogramstakenbytheMDI instrumentonboardSOHO andgivesus13yearsofconsistentdatatoworkwith. A catalogueofactiveregionfragmentshasbeencompletedfortheyear2001, duringthepeakofthelastsolarcycle, andhasallowedustolookatphysicalpropertiesoftheindividualfragments, tracktheirpositionand'propermotion'andexaminetheoverallfragmentdistributions. Wehopetousethecataloguetodeterminepossiblecausesofactiveregionbreakupandlookforanytrendsthatexistinthisprocess. I willpresenttheresultsofthispreliminaryanalysisofthe117,242fragmentsdetected, alongwithsomeideasforfutureuseofthealgorithmsandcatalogue.

P35FIRST Explorer- spacebornelow-frequencyradio

astronomyusingpassiveformationflyingJanBergman (SwedishInstituteofSpacePhysics)

with Richard Blott, Alistair Forbes,David Humphreys, David Robinsson, and

Constantinos Stavrinidis

Space-bornelow-frequencyradioastronomyhasbeenidentifiedasakeyscienceapplicationforaconceptualpathfindermission, usinganovelspace-flightconceptcalled“passiveformationflying”. Themission, FIRST Explorer(Formation-flyingsub-IonosphericRadioastronomyScienceandTechnology), iscurrentlyunderstudybytheEuropeanSpaceAgency(ESA).Itsobjectiveistodemonstratepassiveformation-flyingandtoperformuniquesciencewithaveryhighserendipityfactor, byopeninganewfrequencywindowtoastronomy. Traditionally, formation-flyingrequirescontinuousandminutecorrectionsoftheorbitalelementsandattitudesofthespacecraft. Thisincreasesthecomplexity, andassociatedrisk, ofcontrollingtheformation, whichoftenmakessuchstudiesinfeasiblefortechnologicalandeconomicreasons. Passiveformation-flyingoffersaremedytothoseproblems. Spacecraftinapassiveformationareallowedtodriftandrotateslowly, butbyusingadvancedmetrologyandstatisticalmodellingmethods, theirrelativepositions, velocities, andorientationsaredeterminedwithveryhighaccuracy. Themetrologydataisuseddirectlybytheradioastronomypayloadtocompensateforspacecraftmotionsinsoftware. Thenormallyverystringentspacecraftcontrolrequirementsare

therebyrelaxed, whichsignificantlyreducesmissioncomplexityandcost.

Hydroxidecatalysisbondingresearchforastronomicalapplications

NicolaBeveridge (UniversityofGlasgow)

TheInstituteforGravitationalResearchattheUniversityofGlasgowhasawellestablishedhistoryintheresearchofhydroxidecatalysisbondingforgroundandspacebasedgravitationalwavedetectorapplications. Hydroxidecatalysisbonding, usedtobondsilicasuspensionelementstosilicamirrorsandforbondingsilicaopticstoZerodur, producesstrong, thermallyconductiveandlowlossbonds. Thetechniquecanbeappliedtomanyother(oxide)materialsandisthereforeofinterestforalternativepurposes, includingastronomicalprojectssuchastheExtremelyLargeTelescopewherePZT materialisbondedtosiliconorsiliconcarbide, oropticalfilterapplicationswherecoatedsilicasubstratestocanbebondedontosilicadiscsinordertotransfercoatings. Thispresentationisaimedatgivingabriefoverviewoftheresearchofafewoftheseapplications.

HARMONI - A UK ledfirstlightspectrographfortheE-ELT

FraserClarke (UniversityofOxford)withNiranjan Thatte(PI)

HARMONI isavisible/near-infraredintegralfieldspectrographcurrentlybeingconsideredasoneofthefirstlightinstrumentsforthe42-mEuropeanExtremelyLargeTelescope. HARMONI willprovidemedium-highresolution(R∼ 5000 − 20000)spectroscopyintheV-Kbands(0.47-2.5microns)overanextendedfieldofupto10x5arcseconds. Itwillprovidearangeofpixelsscalesof40mas/pixeltosamplethetelescope'sGLAO correctedPSF,downto4mas/pixeltosamplethediffractionlimitedimagesprovidedbytheATLAS-LTAO system.

I willoutlinethekeysciencecasesforHARMONI,rangingfromextrasolarplanetstohighredshiftgalaxies, alongwiththekeytechnologieswhichwillmakeHARMONI possible.

TheHARMONI consortiumisUK-led(UniversityofOxfordandUKATC),withFrenchandSpanishpartners, andoffersthepossibilityofkeyUKinvolvementintheE-ELT attheveryearliestopportunity. Alongwith7otherinstruments,HARMONI hasrecentlycompletedaphaseAconceptualstudyforESO.

LumpedElementKineticInductanceDetectorssuitableforlargearraysofastronomical

detectors.SimonDoyle (CardiffUNiversity)with

Phil Mauskopf

TheLumpedElementKineticInductanceDetector(LEKID) isasimpletofabricate, superconductingdevicesuitableforuseinlargemultiplexeddetectorarrays. TodatetheLEKID hasdemonstrated200microndetectionofacryogenicblackbodysourceandsuccessfultestingofademonstrationarrayoperatingat2mmontheIRAM telescopeinOctober2009. DuetoitscombinedabsorbinganddetectingelementstheLEKID isanextremelysimpledetectortofabricaterequiringonlyonedepositionandetchsteptoproduceanarrayofupto1000pixelsbeingmultiplexedontoasinglefeed-line. TheLEKID isalsoaverycompactdetectormakingitidealforproducingarrayswithhighfillingfactors. The

suitabilityoftheLEKID foruseinlargearrayshaspromptedareturnvisittotheIRAM telescopewithadualbandinstrumentin2010. ThispresentationwillgiveanoverviewoftheLEKID detectoraswellasitsuseoutsidethemmandsubmmastronomybands.

Milli-kelvincoolerfortheXMS instrumentontheInternationalX-rayObservatory

IanHepburn (UniversityCollegeLondon–MSSL)

Theworldsfirstcryogenfreeflightworthyadiabaticdemagnetisationrefrigeratorforthecoolingofcryogenicdetectorsto50mK wasdeliveredtoESA inJune2008. ThissystemwasdevelopedbyMSSL inassociationwithEADSAstriumundercontracttoESA anddevelopedasatechnologydevelopmentfortheXEUS mission(nowrenamedtheIXO).TheADR wasconstructedasasetofsub-systemsinordertoenablechangesintechnologyandrequirementsatalaterdatetobeintegratedintothesystem. Vibrationqualificationwasperformedonthesub-systemstoAriane5levels.

InthispresentationwepresentdetailsofthedeliveredADR,itssub-systems, theproposed50mK coolerforthecoolingoftheTES detectorsontheX-raymicrocalorimeterspectrometerinstrument(XMS) fortheInternationalX-rayobservatoryandongoingdevelopmentinheatswitchtechnologywhichwillenableacontinuousADR tobeconstructed.

High-PrecisionInterferometryandLow-LossmaterialsforfutureGravitationalWave

ObservatoriesStefanHild (UniversityofGlasgow)

Large-scaleMichelsoninterferometersformthecoreofcurrentandfutureGravitationalWaveAntennas. SincethedaysofAlbertMichelsonandEdwardMorley, thesensitivityofMichelsoninterferometershasbeenimprovedbymorethan12ordersofmagnitude. Tofurtherimproveourabilitytoscantheskyforgravitationalwavesignalsavarietyofinnovativeinterferometrictechniquesandlowlossmaterialsarerequired. Thiswillleadto2ndand3rdgenerationdetectorssuchasAdvancedLIGO andtheEinsteinTelescope.

Thistalkwillsurveycurrent/futuretechniquesininterferometrysuchassqueezedlight, opticalrigidityandotherQuantum-Non-Demolitiontechniques. Furthermore, thepropertiesofSiliconasacryogenicmaterialandthenovelconceptofamonolithicreflectorbasedonmicro-structuredsurfaceswillalsobepresented. Thisallowsthefabricationofhighlyreflectivemirrorswithouttheuseofdifferentmaterials, whichresultsisanopticalcomponentwithalowthermalnoise.

Reducingriskincryogenicinstrumentdesign:thermalconductivitymeasurementsattheCryogenicInstrumentationResearchLab

JuliaKennedy (InstituteforAstronomy, UniversityofEdinburgh)with A.L. Woodcraft

Poorknowledgeofthephysicalpropertiesofmaterialsisaseverelimitationoncryogenicdesign, andasinstrumentsincreaseincomplexitywhilebudgetsshrinkthislackofknowledgeisposinganincreasingrisktocostsandschedules.

Furthermoremanynewmaterials, particularlypolymers, offertheprospectofimprovedperformancebutthereislittleinformationontheircryogenicproperties.

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Unfortunately, veryfewgroupscapableofmakingusefulmeasurementsareabletodevotesignificanttimetodoingso. AttheCIRL (CryogenicInstrumentationResearchLaboratory), wearecarryingoutasystematicprogrammeofmeasurementsofthethermalandelectricalpropertiesofmaterialsfrombelow4K toroomtemperature, concentratingonthoseofuseinlargecryogenicinstruments.

ThesemeasurementsarepartofaUK governmentfundedprogrammetoimprovetheabilitytoconstructcryogenicinstrumentsinbothacademiaandindustry.

Wepresenttheresultsofinitialmeasurementsanddiscussourplansforthenearandlonger-termfuture.

NoveldeformablemirrordevelopmentsforastronomyapplicationsMelStrachan (UKATC)

TheUKATC hasbeencollaboratingisaseriesofprojectsdirectedtowardsaddressingtheadaptiveopticchallengesposedbytheEuropeanExtremelylargetelescope. Wehavedevelopednoveltechnologicalsolutionsforbothlargedeformablemirrorsfortelescopewavefrontcorrection, andminiaturedeformablemirrorsforusewithininstruments. Ourlargedeformablemirrorsurfacematerial, acompliantfromofsiliconcarbide,offersaYoung'sModuluscomparabletoglassbutwithgreater, non-catastrophic, resistancetofracture. Incombinationwiththeextraordinarynewmaterialwehavebeenworkingonanewlow

poweractuatorwithadeflectioncapabilityoftensofmicrons.

AdaptiveopticrequirementsforinstrumentationsuchasEAGLE fortheEuropeanextremelylargetelescopepresentanenormouschallengetodeformablemirrortechnology. Wehavedevelopedauniqueapproachusingfabricatedarraysofmultilayeractuatortechnologytoaddresstherequirementsofactuatordensityanddeflection. Ourprogrammeofworkhasuncoveredanovelapproachwhichhasledtoabuiltintestcapability. Wewillpresenttheoutcomesofourworkwhichwebelievewillleadtoacompactdeformablemirror.

Probingtheatmospheresofextrasolarworldswithadedicatedmissionfromspace

GiovannaTinetti (UCL) with M. Swain,M. Tessenyi, M. Ollivier, G. Vasisht, P. Deroo,J.P. Beaulieu, T. Henning, and THESIS team

TheTHESIS missionconceptisaspace-based,modestcost, lowtechnicalriskmissioncapableofcharacterizingtheatmospheresofexoplanets,includingsuper-Earthsinthehabitablezone.Significantly, THESIS doesnotrequirenewtechnology. BuildingonthesuccessesoftheSpitzerandHubblespacetelescopes, THESISwouldbehighlyoptimizedforsystemstability(1partin 105)andwoulddeliverphoton-noise-limitedspectroscopyandphotometryoverthecrucial0.5–16micronwavelengthrange. Thisrangeofwavelengthscontainssignaturesofwater,methane, ammonia, carbonmonoxide, andnumerousothermolecules, andincludesmoleculesofpotentialprebioticsignificance.

Becausemoleculesserveasprobesofcomposition, conditions, andchemistry, molecularspectroscopyofthedaysideandnightsideregionsofexoplanetatmospheresisthemostpowerfultoolavailableforstudyingtheseobjects. THESISwouldbethefirstmissionexplicitlydesignedtocharacterizeplanetswherelifecouldexist; THESISwouldprofoundlyadvanceourunderstandingofthephysicalconditionsandlikelythehistoriesofexoplanets, rangingfromhot-Jovianstosuper-Earths. THESIS wouldbealow-costUS-Europeanmissionwithenormousdiscoverypotential.

Astronomyatthehighestenergies: theCherenkovTelescopeArray

RichardWhite (UniversityofLeeds)

Very-HighEnergy(VHE) γ−rayastronomyisdominatedbyImagingAtmosphericCherenkovTelescopes(IACTs)andisreliantuponthedetectionofCherenkovradiationfromelectronsincascadesinitiatedbyastrophysical γ−rayshighintheEarth'satmosphere. Resultsfromthelatestgenerationoftelescopes, suchasHESS,MAGICandVERITAS haverevealedaskyrichwithdifferentclassesofVHE object.

StillthelimitsoftheIACT havenotyetbeenreached, andtopushthehigh-energyfrontierofphotonastronomytheCherenkovTelescopeArray(CTA) hasbeenproposed. Comprising50-100IACTsoftwotothreesizes, CTA willprovideanorderofmagnitudeincreaseinsensitivityfrom∼ 3 × 1010 to ∼ 1014 eV.Despitetheextremeenergies, CTA willpossessthebestsensitivityandangularresolutionatanyenergyabovethehardX-rayband.

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Abdulgalil, Ali, 63Achilleos, N., 52Achilleos, Nicholas, 52, 58Agalya, G., 75Agueda, Neus, 68Aguilar-Rodriguez, E., 75Aird, James, 84Akeson, R., 73Al-Salti, Nasser, 59Alexander, C., 54, 85Alexander, Caroline, 48ALFALFA Team, 44Allard, France, 51Allende-Prieto, Carlos, 45Almaini, Omar, 82Anderson, J.P., 46Andrews, D.J., 67Andrews, David, 65Antonova, A.E., 52Arce, H., 63Archontis, Vasilis, 87Argiroffi, C., 84Argo, Megan, 71Arridge, C.S., 58, 66Arridge, Chris, 51, 66Aruliah, A.L., 67Asai, A., 80Aschwanden, M.J., 81ASPERA team, 59Austin, Matthew, 45Avison, Adam, 45Awad, Zainab, 64Aylward, Alan, 79

Bacon, D.J., 50Baddeley, L., 67Badnell, N.R., 80Bagheri, Gemma, 61Bagnulo, Stefano, 84Bailin, Jeremy, 84Baillie, Orsolya, 65Bains, Indra, 73Bains, William, 42Baker, D., 81Baker, Deb, 54Baker, Deborah, 48Baker, Jo, 83Bakunina, I.A., 60Baldry, Ivan, 76Baldry, IvanK., 45Ballai, I., 61Ballai, Istvan, 60Balogh, Andre, 59Barclay, Charles, 85Bareford, Michael, 73Barker, Michael, 78Barlow, M., 51Barlow, MichaelJ., 58Barnsley, Robert, 49Baron, F., 73Baron, Fabien, 72Barr, Ewan, 81Barstow, M.A., 58Basa, S., 57Bassett, B., 77Battaglia, Marina, 68, 88Baugh, C.M., 63Bayet, Estelle, 64, 64, 65Beaulieu, J.P., 90Beggan, C., 79Beggan, Ciaran, 65Benisty, Myriam, 72Bennet, Euan, 58Benson, A., 57Benson, A.J., 63Benson, Kevin, 75Bentley, Robert, 75Bento, Joao, 49

Berger, J.P., 72Bergman, Jan, 89Bernard, J.-P., 78Best, P.N., 44Best, Philip, 44, 63Beswick, R.J., 50Beswick, Rob, 71Beveridge, Nicola, 89Bewsher, D., 54, 81Bewsher, Danielle, 52, 85Bian, Nicolas, 68Bibby, Joanne, 45Bingham, R., 59, 70Binks, A., 73Birch, M.J., 79Birkinshaw, M., 83Bisi, Mario, 75, 87Blake, R., 61Blake, Rob, 54, 62Blanc, AnjaLe, 75Blott, Richard, 89Bluck, Asa, 82Bonfield, Dave, 62Borg, A., 47Bouvier, J., 84Bower, Richard, 77Bradshaw, S.J., 80Bradshaw, Steve, 79Braidwood, L., 48Breen, A.R., 75, 87Bretherton, Claire, 86Brockley-Blatt, C., 54Bromage, B.J.I., 54, 79Bromage, Barbara, 87Brook, C.B., 83Brook, Chris, 56, 84Brook, ChrisB., 45, 84Brooke, John, 54, 75Brookes, Mairi, 63Brown, D.S., 52, 54, 85Brown, John, 68, 70Browne, Ian, 44Browning, P.K., 68Browning, Philippa, 68, 73Brunner, RobertJ., 77Bruno, R., 54Brunthaler, Andreas, 71Bryan, Sarah, 83Buckle, Jane, 46Buffington, A., 75Bulger, J., 84Bulger, Joanna, 63Bunce, E.J., 66Bunclark, Peter, 62Burge, Christina, 68Burke, Claire, 43Burningham, Ben, 77Buscher, D., 73Buscher, David, 72, 72Butters, Oliver, 55Byrne, JasonP., 75

Cairns, R.A., 59, 70Calura, Francesco, 84Cameron, A.C., 55Cameron, Andrew, 42Cameron, AndrewCollier, 73Cameron, Ewan, 44Campusano, L.E., 83Cano, Zach, 70Caputi, Karina, 62Cardoso, Catia, 51Cargill, Peter, 79Carlberg, R., 57Carozzi, Tobia, 55Carpenter, J., 63Carpineti, Alfredo, 43Carr, C.M., 53

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Carr, Chris, 53Caswell, James, 45Cayless, Alan, 55Cecconi, B., 52Cernicharo, J., 51CFHTLenS team, 72Chaizy, P.A., 47Chaplin, W., 86Chapman, S.A., 54Chapman, S.C., 47Chapman, Sean, 64Chapman, Steven, 87Charalambous, A., 67Charnley, Steven, 64Chashei, I.V., 75Che, Xiao, 72Chesneau, Olivier, 72Chiavassa, A., 73Chisham, G., 53Chorley, Nicky, 60Christian, D.J., 87Christian, Damian, 60Christie, Helen, 64Christodoulou, Leonidas, 43Christopher, Natalie, 64Churcher, Laura, 51Cilliers, P., 67Cioni, Maria-Rosa, 61, 61, 62, 79Clark, J.S., 46Clark, James, 82Clark, Simon, 46Clarke, Ellen, 65Clarke, Fraser, 89Clarke, J.T., 52Clementini, Gisella, 62Clements, D.L., 50Clements, David, 49Clilverd, Mark, 65Clover, J.M., 75Clowes, R.G., 83Coates, A.J., 52, 66Coates, Andrew, 66Cole, S., 63Collings, MarkP., 64Collins, C., 43Collins, Ross, 54, 61, 62Colombi, Stephane, 56Conley, A., 57Conselice, Christopher, 82Contursi, A., 64Cooper, Heather, 46Coppin, K., 44Corder, S., 63Cormier, Diane, 64Couchman, Hugh, 84Courty, S., 83Cowley, S.W.H., 52, 65--67Cran-McGreehin, A.P., 70Creech-Eakman, M., 73Crockett, P.J., 87Crockett, Philip, 60, 60Crooker, Nancy, 75Cross, A.W., 59, 70Cross, N., 61Cross, Nicholas, 62Cross, Nick, 54Crothers, S., 53Crowther, Paul, 45Culhane, Len, 48, 54Cunningham, Colin, 42CurtisLake, Emma, 44

daCosta, A.A., 81daCosta, AntonioArmando, 82Dai, Y., 69Dall'Ora, Massimo, 62Dalla, S., 54, 85Dalla, Silvia, 68

Dalton, Gavin, 44Dandouras, I., 47Dandouras, Iannis, 46Darling, Jeremy, 44Dasso, S., 75Davies, B., 46Davies, Ben, 46Davies, J.A., 47, 53, 59, 75, 76, 87Davis, C.J., 59, 76Davis, Chris, 75Davis, Christopher, 75Davis, Gary, 49Davis, Olaf, 56Davs, C.J., 53Dawson, Ewan, 65Day-Jones, Avril, 77DeMoortel, I., 61, 88DeRosa, Robert, 84Deane, Roger, 63DEBRIS consortium, 51Decin, L., 51DeJong, J., 64DelZanna, G., 48, 80DelZanna, Giulio, 48Demoulin, P., 75, 81Demoulin, Pascal, 74DePasquale, Massimiliano, 70Dere, Ken, 87Deroo, P., 90Devriendt, Julien, 56, 83Diamond, Phil, 73Dickinson, Mark, 82Dickson, Ewan, 68Dilday, B., 77Dimbylow, T.G., 47Ding, Jiaoyang, 80Diver, D.A., 82Diver, Declan, 80, 81Diver, DeclanA., 58, 80Dominguez, SantiagoVargas, 48Donati, J.-F., 84Donati, Jean-Francois, 73Dorrian, G.D., 87Dorrian, Gareth, 87Dougherty, M.K., 66, 67Dougherty, Michele, 53Dougherty., M.K., 52Down, Emily, 83Doyle, Gerry, 51Doyle, J.G., 52, 76, 80, 81Doyle, Simon, 89Driel-Gesztelyi, Lidiavan, 74Driver, Simon, 44Dufour, P., 58Dunlop, J.S., 44Dunlop, James, 62Dunlop, Jim, 63Dunlop, M.W., 47Duthie, Roger, 46

e-MERGE consortium, 63Eastwood, Jonathan, 47Edberg, N.J.T., 67Efstathiou, George, 42Egami, E., 56Eke, V.R., 57Eldridge, John, 78Ellis, Richard, 78Elsworth, Y., 86Emerson, Jim, 62Erdélyi, R., 60, 61, 86ESA,50Escoubet, C.Philippe, 47Escoubet, C.P., 47Espinoza, Cristobal, 81Evans, A., 46Evans, Christopher, 46Evans, D.A., 83

Eyles, C.J., 52, 53Eymeren, Janinevan, 71Eyres, S.P.S., 46

Falcke, H., 50Falder, James, 83Fallows, R.A., 75, 87Famaey, Benoit, 72, 84Farihi, Jay, 58Fazakerley, A.N., 47, 48, 54, 76Fazakerley, Andrew, 46Fear, Robert, 74Fedeli, Cosimo, 71Feigelson, E.D., 84Feix, Martin, 71, 72, 84Fender, R., 50Fenech, Danielle, 71Ferdman, Robert, 82Ferguson, A., 78FermiGBM Collaboration, 70Ferreras, Ignacio, 44, 56, 78Findlay, Joseph, 62Finger, Lars, 63Fischer, J., 64Flaccomio, E., 84Fletcher, Lyndsay, 48, 69, 80, 89Fludra, Andrzej, 53, 53FMOS team, 44Folsom, C., 84Forbes, Alistair, 89Forgan, Duncan, 55Fornacon, K-H., 47Forsyth, C., 47, 48Forsyth, Colin, 47Forsyth, RobertJ., 59Fossati, L., 84Fouchez, D., 57Foullon, C., 88Frankland, Victoria, 64Franz, M., 67Fraser, Morgan, 70Freeman, M.P., 53Frenk, C.S., 63Frenk, Carlos, 56Freytag, B., 73Fujihara, Gary, 86Fujiki, K., 75Fullekrug, Martin, 66Fuller, G,50Fuller, Gary, 45, 64, 64, 65

Gerard, J.-C., 52Gaensicke, Boris, 76GalaxyZooteam, 43, 55GALEX Collaboration, 78Gallagher, Peter, 75Gallagher, PeterT., 88Galsgaard, K., 74, 80Galsgaard, Klaus, 74GAMA Team, 43--45Garrett, M., 50Garrington, Simon, 49, 71Garza, K., 47Gaunt, C.T., 67Geach, Jim, 44, 77Geballe, T.R., 46Geen, Sam, 83Gentile, Gianfranco, 72Genzel, R., 64Getman, K.V., 84Ghodsi, Hoda, 56Gibson, B.K., 83Gibson, Brad, 84Gibson, BradK., 45Gillespie, K.M., 59, 70Gilmore, G., 57Giunta, A.S., 75Glubokova, S.K., 75

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Goldstein, M., 47Gombosi, T.I., 85Gonzalez-Esparza, A., 75Gonzalez-Solares, Eduardo, 62GordonEmslie, A., 69Gordon, James, 72Gordon, K.D., 78Gordovskyy, Mykola, 68Gough, D., 86GraciaCarpio, J., 64Grady, Keith, 69, 69Graham, David, 48Graham, M.J., 83Grande, M., 59, 67Granot, Jonathan, 70Gray, Norman, 55Greaves, Jane, 51Green, James, 45Green, L.M., 85Green, Lucie, 48, 54, 85Green, LucieM., 74Gregory, Scott, 84Grey, Malcolm, 73Griffin, E.M., 67Griffin, Matt, 50Grocott, A., 47, 52Grocott, Adrian, 66Grocutt, Emma, 72Grodent, D., 52Guandalini, Roald, 62Guio, P., 52, 58Guo, Jingnan, 69Gupta, Jennifer, 44Gürkan, Gülay, 71

H-ATLAS team, 51Haas, M., 64Habergham, Stacey, 46Haberzettl, L., 83Hailey-Dunsheath, S., 64Haines, C., 56Hall, Elizabeth, 63Hallinan, G., 52Hallinan, Gregg, 51Hambly, N., 61Hambly, N.C., 58Hambly, Nigel, 54, 55, 62Hamilton-Morris, Victoria, 56Hammond, Giles, 85Hancock, B.K., 54Haniff, C., 73Haniff, C.A., 73Haniff, Chris, 72Hannah, Iain, 48, 68, 69, 88Hapgood, M.A., 47Hapgood, Mike, 47, 53, 75Hara, H., 48Hardcastle, M., 83Hargreaves, John, 79Harniman, R., 77Harper, Graham, 73Harra, L.K., 48, 76Harra, Louise, 54Harra, LouiseK., 49Harris, Jennifer, 88Harris, Kathryn, 83Harrison, Michael, 74Harrison, Richard, 53Harrison., R.A., 76Harvey, Janice, 86Hatchell, Jennifer, 42Haubois, X., 73Haynes, Andrew, 74He, W., 59Heald, George, 50Heavens, Alan, 72Hebden, Kerry, 64Heinke, CraigO., 82

Heinzel, P., 88Hellier, C., 42, 55Hempel, M,62Hendry, Martin, 57, 85Hendry, MartinA., 56, 57, 82Heng, IkSiong, 82Henning, T., 90Hepburn, Ian, 89HerMES Consortium, 51HerschelMESS Keyprojectconsortium, 58HESS Collaboration, 82HeViCS Consortium, 51Heyden, Kurtvander, 50Heyer, Inge, 86Heymans, Catherine, 72Heywood, Ian, 63Hick, P.P., 75HIFI consortium, 50Higgins, Paul, 88Hild, Stefan, 89Hill, David, 44, 44Hillier, Dan, 86Hnat, B., 47, 60Ho, Wynn, 82Hoare, M.G., 46Hodgkin, Simon, 62Hodgson, Lisa, 63Hoekstra, Henk, 71, 72Holliman, M., 61Holliman, M.S., 55Holliman, Mark, 54, 55Holme, Richard, 66Homeier, Derek, 51Honary, F., 67, 79Hood, A.W., 88Hood, Alan, 48Hood, AlanW,87Hook, I., 57Horbury, Tim, 75Horn, Markus, 57Horne, RichardB., 79Hornig, Gunnar, 74, 74House, Elisa, 83HowelI,V.S.C., 67Howell, D.A., 57Hoyle, B., 50Hsieh, Henry, 58Huang, Zhenghua, 80Hudson, Hugh, 60, 80Humphreys, David, 89Humphries, Thomas, 65Hussain, G.A.J., 84Hussain, Gaitee, 85Hutcheon, Richard, 78Hutchinson, James, 66Hutchinson, M.G., 47Huxor, Avon, 55, 77

Ibar, Edo, 44Ibata, R., 78Ibrahimov, M., 84Indebetouw, R., 78Inglis, A.R., 60Irwin, M., 78Irwin, Mike, 62Isella, A., 72Ivanov, V,62Ivison, R.J., 44Izzo, C., 84

Jackson, B.V., 75Jackson, Brendan, 57Jackson, Neal, 71Jackson, Richard, 85Jaffe, Andrew, 76Jain, R., 86Jain, Rekha, 74JamesMcAteer, R.T., 75, 88

James, P.A., 46James, PhilA., 45Jansari, Kishan, 61Jardine, M., 84Jardine, Moira, 52Jarvis, Matt, 50, 62, 83Jatenco-Pereira, V., 85Jeffrey, Natasha, 88Jeffries, Rob, 85Jensen, E.A., 75Jess, D.B., 87Jess, David, 60, 60JodcastTeam, 86John, Daniel, 57Johnson, Olivia, 86Johnston, Russell, 44Jones, Geraint, 59, 66Jones, GeraintH., 59Jones, Hugh, 77Jones, Mark, 55Jones, Olivia, 78Jonsson, Jakob, 57Josselin, E., 73Jurgenson, C., 73

Kanani, Sheila, 66Kataria, D.O., 54Kavanagh, A.J., 68Kaviraj, S., 43Kaviraj, Sugata, 78Kawata, Daisuke, 45Kay, ScottT., 83Keenan, F.P., 87Keenan, Francis, 60Kellett, B.J., 52, 59, 70Kellett, Stephanie, 66Kelly, Gemma, 66Kelly, J., 54, 85Kelvin, Lee, 44, 44Kemper, Ciska, 64Kemper, F., 78Kennedy, Grant, 51Kennedy, J., 75Kennedy, Julia, 89Keogh, Dominic, 82Ker, Louise, 63Khotyainstev, Yu. V., 47Kidd, Robert, 59Kiessling, Alina, 72Kim, Hansik, 63King, Robert, 51Kipping, David, 58Kirk, J.M., 51Kistler, L., 47Kitching, Tom, 72Kivelson, M.G., 52Kiyani, Khurom, 47Klaas, U., 64Klockner, Hans-Rainer, 63Kochukhov, O., 84Koda, J,63Kontar, E.P., 48, 69Kontar, Eduard, 68--70, 88Kosch, M., 67Kosch, M.J., 67Kotze, P., 67Kraemer, K.E., 78Kraft, R.P., 83Kramer, M., 82Kraus, Stefan, 72Krause, O., 64Kukula, Marek, 75, 86Kunawicz, Nadya, 65Kurtz, Donald, 86Kuznetsov, Alexey, 51

Laakso, H., 47Laatsch, Shawn, 86

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Labrosse, Nicolas, 88Lacerda, Pedro, 58Lacey, C.G., 63Lagadec, E., 78Laing, E.W., 81, 82Laird, Elise, 82, 84Lampeitl, H., 77Lamy, L., 52, 65, 67Landstreet, J.D., 84Lang, Pauline, 52Langer, Norbert, 78LAT Collaboration, 70Lavraud, B., 47Lavraud, Benoit, 75Lawrence, Andy, 63Lawrie, Craig, 57LeBlanc, Anja, 54Leech, Jamie, 45Leier, Dominik, 78Leland, B., 84Lemke, D., 64Lester, M., 47, 66, 67Lester, Mark, 53, 66Levan, A., 71Levan, A.J., 71Levan, Andrew, 82Lewis, G., 78Lewis, Gethyn, 66Lewis, James, 62Li, Baojiu, 72Li, Chuan, 69Li, Xing, 88Liang, Guiyun, 80LIGO ScientificCollaboration, 71Lim, Jeremy, 73Lin, Bob, 42Linden, RonaldVander, 73Lindsey, C.A., 60Linker, J.A., 75Lintott, Chris, 55, 75Linz, H., 64Littlefair, Stuart, 52Liu, Siming, 69, 69Livi, S., 54LOFAR imagingcommissioningteam, 50Logue, Joshua, 57Lotz, S.I., 67Louarn, P., 54Loveday, Jon, 43, 77Lowe, Stuart, 86Lu, Q.M., 80Lucas, Philip, 62Lucek, E., 47Lucek, Elizabeth, 46, 53, 53Lui, A., 47Lumsden, S.L., 46Luna, Marialejandra, 60Lutz, D., 64Lykou, Foteini(Claire), 72Lyne, A., 82Lyne, A.G., 81

Maccio, Andrea, 72Macdonald, Erin, 44Macintosh, B., 84Mackay, D.H., 76, 80MacKinnon, A.L., 52MacKinnon, Alec, 68, 70, 86MacLachlan, CraigS., 80Maclean, R.C., 48Maclean, Rhona, 74MacTaggart, David, 88Madden, S., 64Madjarska, M.S., 76, 80, 81Madjarska, Maria, 80, 81Majewski, Pawel, 57Malbet, F., 72Mallik, Procheta, 80

Maloney, ShaneA., 75Mandrini, C.H., 81Mandrini, Cristina, 74Mann, R.G., 55, 61Mannering, Elizabeth, 83Manoharan, P.K., 75Mao, Shude, 83Marconi, Marcella, 62Marcu, A., 61Marengo, M., 78Maria, Anna, 69Marin, Felipe, 77Markwick, Andrew, 65Marquette, Jean-Baptiste, 62Marsden, Richard, 54Marsh, M., 48, 54, 85Marsh, Mike, 60Marsh, T.R,77Martin, S., 64Martin-Pintado, J., 64Martinez-Oliveros, J.C., 60Mason, Andrew, 46Mason, H., 80Mason, H.E., 85Mason, Helen, 49, 86, 88Massi, F., 72Masson, A., 47Massone, and, 69Massone, AnnaMaria, 56Masters, Adam, 52Mathioudakis, M., 87Mathioudakis, Mihalis, 60Matsuura, M., 51, 78Matsuura, Mikako, 58Matthews, Brenda, 51Matthews, S.A., 69Matthews, Sarah, 48, 74Matthews, SarahA., 74Mauch, Thomas, 44Mauskopf, Phil, 89Mawson, Neil, 49Maxted, P.F.L., 78Mayer, L., 57McCaughrean, Mark, 42McCaughrean, MarkJ., 51McClements, K.G., 88McConnachie, A., 57McConville, S.L., 59, 70McCord, K., 73McCoustra, Martin, 63, 65McCoustra, MartinR.S., 64McCracken, T., 73McCrea, I., 67McDermott, A., 47McDonald, I., 78McHardy, Ian, 63McKean, John, 50McKinnell, L.-A., 67McLaughlin, James, 88McLay, Sam, 65McMahon, Richard, 62McQuillin, Rachael, 83McWhirter, I., 67Meixner, M., 78Melrose, Don, 43MESS consortium, 51Messineo, M., 46Meyer, Karen, 80Michaud, Peter, 86Middleton, H.R., 67Miki, Z., 75Milan, S.E., 47, 53, 66, 67, 76Milan, Steve, 74Millar, Tom, 65Miller, David, 72Miller, Grant, 85Miller, Steve, 59Minnitti, D,62

Mitchell, Cathryn, 67MitraKraev, Urmila, 80MMB Collaboration, 45Monnier, John, 72, 73Moretti, MariaIda, 62Morgan, H., 75Moro-Martin, Amaya, 51Mortlock, Daniel, 76Morton, Richard, 60, 86Mouikis, C., 47Murphy, David, 77MUSYC Collaboration, 78Muxlow, T,50Muxlow, T.W.B., 50Muxlow, Tom, 63, 71Myers, AdamD., 77Ménard, F., 72

Nakariakov, V.M., 60, 88Nandra, Kirpal, 82, 84Natta, A., 72Negueruela, I., 46Nelson, Richard, 43Neukirch, Thomas, 59, 69, 74New, R., 86NGLS teammembers, 45Ngwira, C.M., 67Nicerkson, Sarah, 84Nichol, R., 50, 77Nichol, Robert, 77Nichols, Jonathan, 52Nielbock, M., 64Nishino, M.N., 47Norton, A.J., 46Nutter, David, 49Nykyri, K., 47

O'Brien, P.T., 71O'Dwyer, Brendan, 88O'Neil, Robert, 49Oieroset, M,47Olivares, A., 73Ollivier, M., 90Opher, M., 85Opperman, B., 67Orza, Beniamin, 61Oudmaijer, R.D., 46Oudmaijer, Rene, 72Owen, C.J., 47, 48, 69, 75Owen, Christopher, 54Owens, M.J., 75Owens, Mathew, 75Owens, Steve, 87

PACS consortium, 50Parnell, Clare, 74Parsons, H., 46Pascoe, David, 61Pastorello, A., 70Patel, Harsit, 50Patel, Prina, 50Patience, J., 63, 84Patience, Jenny, 51, 73Peacock, John, 57, 63Pearson, J., 54Pedlar, Alan, 71Pedram, Ehsan, 74Pedretti, E., 73Pedretti, Ettore, 73Penarrubia, Jorge, 57Penny, Alan, 50Percival, Susan, 79Percival, WillJ,77Perlman, E.S., 83Perrett, K., 57Perrin, G., 73Perry, Chris, 75Persoon, A.M., 66

94

Pestaña, JoséLuisGarrido, 71Petit, Pascal, 73Petkaki, Panagiota, 68Petrosian, V., 63Phan, T.D., 47Phelps, A.D.R., 59, 70Phillipps, S., 55, 77Phillips, Neil, 51Piana, Michele, 56, 69Pilkington, Kate, 84Pinfield, David, 77Pintér, B., 75Pitkin, Matthew, 82, 82Plez, B., 73Poglitsch, A., 64Polehampton, E., 51Polehampton, E.T., 58Pollacco, D., 42, 55Pontin, David, 74, 74Pontin, DavidI., 74Pope, A., 44Popescu, CristinaC., 45Popescu, M., 85Potts, Hugh, 80Potts, HughE., 80Power, C., 63Predoi, Valeriu, 71Prescott, Matthew, 45Price, J., 77Priest, E.R., 74Prinja, Raman, 45Pritchet, C., 57Provan, G., 65Provan, Gabby, 67Pryse, S.E., 59, 67Pu, Z., 47

Rae, I.J., 47Raeder, Joachim, 74Rahimi, Awat, 45Rangel, Cyprian, 84Ratcliffe, Heather, 69Rawlings, Steve, 50, 63, 83Rea, Alex, 73Reach, W.T., 78Read, Justin, 57Read, M., 61Read, M.A., 55Read, Mike, 54, 55, 62Reay, Sarah, 65Redfield, S., 58Reid, H.A.S., 69Reid, Hamish, 69Rekjuba, M,62Relano, Monica, 78Rhodes, R., 73Rice, Ken, 55Richards, Anita, 58, 73Richer, J.S., 46Richer, John, 50Rigby, Emma, 51, 63Rigopoulou, Dimitra, 45, 50Riley, P., 75Ripepi, Vincenzo, 62RMS Team, 46Roberts, Helen, 65Robertson, C.W., 59Robertson, David, 61Robinson, Terry, 67Robinsson, David, 89Robotham, Aaron, 44, 45Roche, P., 46Rodger, Craig, 65Ronald, K., 70Ronald, Kevin, 59Rosa, RobertDe, 51Ross, Ashley, 77Ross, Nicholas, 77

Roth, M., 86Rottgering, Huub, 63Rouillard, Alexis, 75Rowlinson, Antonia, 71Roxburgh, I., 86Ruderman, M.S., 61Ruffle, Paul, 65Rushton, M.T., 46Rushton, Mark, 46Ryans, R.S.I., 87Rycroft, Michael, 66

Sabiu, Cristiano, 77SAGE-Specteam, 79Saha, Prasenjit, 78Sahraoui, F., 47Saito, R,62Sakai, Satoru, 82Salucci, Paolo, 72Sanchez-Blazquez, P., 83Sanderson, A., 56Santoro, F., 73Sargent, A., 63Sargent, B.A., 78Sathyaprakash, Bangalore, 43Saunders, Richard, 63Sauvage, M., 64Schawinski, Kevin, 78Schinnerer, E., 64Schmieder, B., 88Schneider, M., 63Schreiber, J., 64Schwadron, Nathan, 75SDSS-II SNeSurveyTeam, 77SDSS-III:BOSS Team, 77Semionov, Dmitrij, 45Senior, A., 68Senior, Andrew, 67Sergis, N., 66Sharples, Ray, 50ShaunBloomfield, D., 88Shay, M.A., 47Sheldon, ErinS., 77Shelyag, S., 61Shelyag, Sergiy, 60Shen, C., 47Shetty, Vineeth, 75Shi, J., 47Shishov, V.I., 75Shtromberg, A., 73Sibbons, Lisette, 79Sibeck, David, 74Sibthorpe, Bruce, 51Silk, Joe, 56Silk, Joseph, 78Simpson, Fergus, 57Singal, S., 63Sivasankaran, Anoop, 56Sivia, Devinder, 83Sloan, G.C., 78Slyz, Adrianne, 83Smail, Ian, 44, 63Smartt, S., 70Smecker-Hane, T., 78Smith, Anthony, 51Smith, Arfon, 55Smith, G.P., 56Smith, James, 55Smith, Mathew, 77Smith, Matthew, 51Smith, Rachel, 73Smith, Russell, 79Sobral, David, 44Sochting, I.K., 83Southwood, David, 52Spain, Timothy, 67, 79Speck, A.K., 78Speirits, Fiona, 57

Speirs, D.C., 59Speirs, David, 70Spencer, P,67SPIRE consortium, 50Stallard, Tom, 59Stamatellos, D., 51Stanway, Elizabeth, 78Stappers, B., 82Stark, C.R., 81Stark, C.R., 82Stark, Craig, 70Stavrinidis, Constantinos, 89Stawarsz, L., 63Steed, Kimberley, 75Steeghs, D., 77Steele, I.A., 49Steele, Iain, 49Sternberg, A., 64Stevens, Jason, 83Steves, Bonnie, 56Stinson, Greg, 84, 84Stott, J., 43Strachan, Mel, 90Sturm, E., 64Subramanian, Srividya, 76, 81Sullivan, M., 57Sullivan, Mark, 71Sun, Jian, 54sunearthplan.netteam, 87Suntrekteam, 86Sutherland, Will, 62, 62Sutorius, E., 61Sutorius, Eckhard, 54, 62Swain, M., 90Sweatman, Winston, 56SwiftTeam, 70Swinyard, B., 52Swinyard, BruceM., 58

Tacconi, L., 64Takato, Naruhisa, 44Takats, K., 70Tamura, Naoyuki, 44Tan, BoonKok, 45Tang, Y.H., 69Tanvir, N., 78Tanvir, N.R., 71Tanvir, Nial, 43Targett, T., 56Taroyan, Y., 61Tatton, Bejamin, 79Tatulli, E., 72Taylor, Andy, 72Taylor, M.G.G.T., 47Taylor, Matt, 47Teodoro, L.F.A., 57, 81, 82Teodoro, LuisF.A., 57, 58Tessenyi, M., 90Th. vanLoon, J., 78Thatte, Niranjan, 89THESIS team, 90Thompson, M., 46, 86Thompson, M.J., 61Thomson, A.W.P., 67, 79Thomson, Alan, 66Thomson, AlanP,65Thomson, andAlan, 65Thomson, Edward, 57Threlfall, James, 88Tideswell, David, 65Tielens, A.G.G.M., 78Tinetti, G., 58Tinetti, Giovanna, 90Tokumaru, M., 75Tout, Christopher, 78Tripathi, Durgesh, 49Trotta, Roberto, 76Trung, Dinhvan, 73

95

Tsiklauri, David, 81Tuffs, RichardJ., 45Tunnicliffe, Rachel, 71Turkmani, Rim, 70Turnbull, Katie, 79Turner, A., 47Tyul’bashev, S.A., 75

UltraVISTA consortium, 62Usuda, KumikoS., 86

vanBallegooijen, A.A., 76, 80VanDoorsselaere, Tom, 61vanDriel-Gesztelyi, Lidia, 76, 81vanSpaandonk, Lieke, 77Vanninathan, Kamalam, 81VargasDominguez, Santiago, 49Vasisht, G., 90Vekstein, G.E., 68Verma, A., 64Verth, G., 60Verth, Gary, 61Verwichte, E., 88VHS collaboration, 62Vickers, Hannah, 67VIDEO Consortium, 62Vidotto, Aline, 85Vigroux, L., 64VIKING Team, 62VirgoCollaboration, 71Viti, S., 64Viti, Serena, 64Vlahos, Loukas, 70VMC Team, 61, 62Volwerk, M., 47Vorgul, I., 59, 70

Wadsley, James, 84Waldmann, Ingo, 58Walker, Helen, 87Walker, M., 57Walker, Matthew, 57Wall, Jasper, 63Wallace, Alison, 74, 87Walsh, A.P., 47, 75

Walsh, Andrew, 48Walsh, R.W., 48, 60, 85Walsh, Robert, 54Walter, F., 64Walter, F.M., 84Wang, Yougang, 84Ward, Martin, 71Ward-Thompson, Derek, 51Wardle, Nick, 61WASP Consortium, 42WASP Consortium, 55Watanabe, T., 48Waterson, Natasha, 75Watson, Fraser, 89Watson, Laura, 76Watt, C., 47Weltevrede, P., 82Weltevrede, Patrick, 59Wesson, Roger, 51, 58West, R., 42West, R.G., 55Westmoquette, Mark, 84Whaler, Kathy, 43Wheatley, Peter, 49White, G.J., 52White, Richard, 90Whitley, Toby, 66Whyte, C.G., 59Wiersema, K., 71Wilcock, L., 51Wild, J.A., 53, 59, 68, 79Wild, J.M., 85Wild, Jim, 67, 87Wilkins, G.M.H., 85Williams, Anthony, 67, 76Williams, D.A., 64Williams, David, 54Williams, DavidR., 49Williams, P., 61Williams, Peredur, 54Williger, G.M., 83Wilmot-Smith, Antonia, 74, 74Wilson, Fiona, 74Wilson, R.J., 66Wise, M., 50

Wit, W.-J.de, 46Witherick, Dugan, 58Woan, Graham, 55, 82Wood, A.G., 75Wood, Alan, 59, 67Woodcraft, A.L., 89Woodfield, Emma, 68Woods, P.M., 78Woods, Paul, 79Worrall, D.M., 83Wright, A.N., 61, 70Wright, Andrew, 70Wright, D.M., 66Wright, Gillian, 43Wu, Xufen, 84Wyatt, M.C., 73Wyatt, Mark, 51Wyper, Peter, 74Wyse, Rosie, 43

Yates, Japheth, 52Yates, Jeremy, 73Yates, JeremyA., 58Yeates, Anthony, 74, 76Yeates, AnthonyR., 74Yeche, Christophe, 77Yeoman, T.K., 53, 66Yi, Sukyoung, 78Yiu, H.-C.I., 67Young, Dave, 66Young, J., 73Young, John, 72, 73Young, Neil, 82Young, P., 48Young, Peter, 49Yu, Shenghua, 52

Zanna, GiulioDel, 49, 61, 88Zarka, P., 52Zezas, Andreas, 71Zhang, ZengHua, 77Zhao, Hongsheng, 71, 72, 84Zharkov, Sergei, 61Zijlstra, Albert, 72

96

List

of p

artic

ipan

tsAbdulgalil, Ali(Heriot-WattUniversity)

agma1@hw.ac.uk [P17]Abernathy, Matthew(UniversityofGlasgow)

m.abernathy@physics.gla.ac.ukAchilleos, Nicholas(UCL) nick@apl.ucl.ac.uk

[P13, P08]Aerts, Conny(UniversityofLeuven)

conny@ster.kuleuven.beAlexander, Caroline(UCLAN)

calexander@uclan.ac.uk [P04]Ames, Susan(OxfordAstrophysics)

sames@astro.ox.ac.ukAndrews, David(UniversityofLeicester)

dja13@ion.le.ac.uk [P18]Anthony, Caroline(ImperialCollege)

c.anthony09@imperial.ac.ukArchontis, Vasilis(UniversityofStAndrews)

vasilis@mcs.st-and.ac.uk [P34]Arridge, Chris(MSSL /UCL) csa@mssl.ucl.ac.uk

[P18, P08]Austin, Matthew(UCL) mja@star.ucl.ac.uk [P02]Avison, Adam(JodrellBankCentrefor

Astrophysics) aavison@jb.man.ac.uk [P02]Awad, Zainab(Dept.ofPhysicsandAstronomy,

UCL) zma@star.ucl.ac.uk [P17]Badnell, Nigel(UniversityofStrathclyde)

badnell@phys.strath.ac.ukBagheri, Gemma(UniversityofHertfordshire)

g.bagheri@herts.ac.uk [P15]Bagnulo, Stefano(ArmaghObservatory)

sba@arm.ac.uk [P32]Bailey, Mark(ArmaghObservatory) meb@arm.ac.ukBains, William(RufusScientific/MIT)

william@williambains.co.uk [Plenary]Baldry, Ivan(LiverpoolJMU)

ikb@astro.livjm.ac.uk [P26]Ballai, Istvan(UniversityofSheffield)

i.ballai@sheffield.ac.uk [P14]Barclay, Charles(MarlboroughCollegeandOxford

Astrophysics) ceb@marlboroughcollege.org[P33]

Bareford, Michael(TheUniversityofManchester)michael.bareford@postgrad.manchester.ac.uk[P23]

Barker, Michael(RoyalObservatoryEdinburgh)mkb@roe.ac.uk [P27]

Barnsley, Robert(LJMU) rmb@astro.livjm.ac.uk[P05]

Baron, Fabien(UniversityofMichigan)fbaron@umich.edu [P22]

Barr, Ewan(MPIfR Bonn)ebarr@mpifr-bonn.mpg.de [P30]

Bartlett, Jo(UCL/MSSL) jb2@mssl.ucl.ac.ukBaruah, Leon(UniversityofSussex)

l.baruah@sussex.ac.ukBassiri, Riccardo(UniversityofGlasgow)

r.bassiri@physics.gla.ac.ukBattaglia, Marina(UniversityofGlasgow)

mbattaglia@astro.gla.ac.uk [P19, P34]Bayet, Estelle(UCL) eb@star.ucl.ac.uk [P17, P17,

P17]Beaulieu, Jean-Philippe(UniversityCollegeof

London) beaulieu@iap.frBeggan, Ciaran(BritishGeologicalSurvey)

ciar@bgs.ac.uk [P18]Benisty, Myriam(INAF -Arcetri)

benisty@arcetri.astro.it [P22]Bennet, Euan(UniversityofGlasgow)

e.bennet@astro.gla.ac.uk [P13]Bentley, Robert(UCL-MSSL) rdb@mssl.ucl.ac.uk

[P24]Bento, Joao(UniversityofWarwick)

joao.bento@warwick.ac.uk [P05]Bergman, Jan(SwedishInstituteofSpacePhysics)

jb@irfu.se [P35]Berry, Christopher(InstituteofAstronomy,

UniversityofCambridge) cplb2@cam.ac.uk

Best, Philip(IfA Edinburgh) pnb@roe.ac.uk [P16,P01]

Beveridge, Nicola(UniversityofGlasgow)n.beveridge@physics.gla.ac.uk [P35]

Bewsher, Danielle(UniversityofCentralLancashire) dbewsher@uclan.ac.uk [P09, P33]

Bian, Nicolas(UniversityofGlasgow)nbian@hotmail.com [P19]

Bibby, Joanne(UniversityofSheffield)j.bibby@sheffield.ac.uk [P02]

Birch, Martin(UniversityofCentralLancashire)mjbirch@uclan.ac.uk

Bird, Anthony(SAF) tonybirdapb@hotmail.comBisi, Mario(AberystwythUniversity)

Mario.Bisi@aber.ac.uk [P99, P24, P34]Blake, Rob(RoyalObservatoryEdinburgh)

rpb@roe.ac.uk [P15, P10]Bluck, Asa(UniversityofNottingham)

ppxab3@nottingham.ac.uk [P31]Boles, Tom(CoddenhamObservatory)

tomboles@coddenhamobservatories.orgBromage, Barbara(JeremiahHorrocksInstitute,

UCLan) bjibromage@uclan.ac.uk [P34]Bromage, Gordon(JeremiahHorrocksInstitute,

UCLan) gebromage@uclan.ac.ukBrook, Chris(UniversityofCentralLancashire)

cbbrook@uclan.ac.uk [P11, P31]Brooke, John(UniversityofManchester)

john.brooke@manchester.ac.uk [P24, P10]Brown, Daniel(UniversityofCentralLancashire)

DSBrown@uclan.ac.ukBrown, John(UniversityofGlasgow)

john@astro.gla.ac.uk [P19, P19]Browne, Paul(UniversityofStAndrews)

pb337@st-andrews.ac.ukBrowning, Philippa(JBCA,Universityof

Manchester) p.browning@manchester.ac.uk[P19, P23]

Bruce, Victoria(IfA,UniversityofEdinburgh)vab@roe.ac.uk

Bryan, Sarah(UniversityofManchester)sarah.bryan@gmail.com [P31]

Buckle, Jane(UniversityofCambridge)j.buckle@mrao.cam.ac.uk [P02]

Bulger, Joanna(UniversityofExeter)joanna@astro.ex.ac.uk [P16]

Burge, Christina(UniversityofGlasgow)c.burge@astro.gla.ac.uk [P19]

Burke, Claire(AstrophysicsResearchInstituteLJMU) cb@astro.livjm.ac.uk [P01]

Buscher, David(UniversityofCambridge)dfb@mrao.cam.ac.uk [P22, P22]

Butters, Oliver(UniversityofLeicester)ob30@star.le.ac.uk [P10]

Calura, Francesco(JeremiahHorrocksInstitute,UCLAN) fcalura@oats.inaf.it [P31]

Cameron, Andrew(UniversityofStAndrews)acc4@st-and.ac.uk [Plenary]

Campsie, Paul(UniversityofGlasgow)p.campsie@physics.gla.ac.uk

Cano, Zach(ARI,JohnMooresUniversityLiverpool) zec@astro.livjm.ac.uk [P20]

Cargill, Peter(ImperialCollege)p.cargill@imperial.ac.uk [P29]

Carozzi, Tobia(Univ.ofGlasgow)t.carozzi@astro.gla.ac.uk [P10]

Carpineti, Alfredo(ImperialCollege)alfredo.carpineti07@imperial.ac.uk [P01]

Carr, Chris(ImperialCollegeLondon)c.m.carr@ic.ac.uk [P09]

Chaplin, William(UniversityofBirmingham)wjc@bison.ph.bham.ac.uk

Chapman, Bob(UniversityofIceland)bob.chapman@physics.org

Chapman, Sean(UniversityofManchester)sean.chapman@manchester.ac.uk [P17]

Chapman, Steven(UniversityofCentralLancashire) sachapman@uclan.ac.uk [P34]

97

Charnley, Steven(NASA GoddardSpaceFlightCenter) Steven.B.Charnley@nasa.gov [P17]

Chorley, Nicky(UniversityofWarwick)n.d.y.chorley@warwick.ac.uk [P14]

Christie, Helen(UniversityCollegeLondon)hc@star.ucl.ac.uk [P17]

Christodoulou, Leonidas(UniversityofSussex)L.Christodoulou@sussex.ac.uk [P01]

Christopher, Natalie(UniversityofOxford)natalie.christopher@astro.ox.ac.uk [P17]

Chrysostomou, Antonio(JointAstronomyCentre)a.chrysostomou@jach.hawaii.edu

Cioni, Maria-Rosa(UniversityofHertfordshire)M.Cioni@herts.ac.uk [P27, P27, P15, P15,P15]

Clark, Simon(OpenUniversity)s.clark@open.ac.uk [P02]

Clarke, Ellen(BritishGeologicalSurvey)ecla@bgs.ac.uk [P18]

Clarke, Fraser(UniversityofOxford)fraser.clarke@physics.ox.ac.uk [P35]

Clements, David(None) d.clements@ic.ac.uk[P05]

Clowes, Roger(Univ.ofCentralLancashire)rgclowes@uclan.ac.uk

Clube, Kim(RoyalAstronomicalSociety)kc@ras.org.uk

Collings, Mark(Heriot-WattUniversity)m.p.collings@hw.ac.uk

Collins, Ross(IfA,Edinburgh) rsc@roe.ac.uk [P15,P15, P10]

Cooper, Heather(UniversityofLeeds)pyhdc@leeds.ac.uk [P02]

Cossham, Jennifer(JohnWiley&Sons, Ltd)jcossham@wiley.com

Crockett, Philip(Queen'sUniverstyBelfast)pcrockett02@qub.ac.uk [P14, P14]

Cross, Nicholas(IfA,Edinburgh) njc@roe.ac.uk[P15]

Crowther, Paul(UniversityofSheffield)Paul.Crowther@sheffield.ac.uk [P02, P27]

Culhane, Len(MSSL/UCL) jlc@mssl.ucl.ac.uk[P04, P09]

Cunningham, Colin(UK AstronomyTechnologyCentre) colin.cunningham@stfc.ac.uk[Plenary]

CurtisLake, Emma(UniversityofOxford)efcl@astro.ox.ac.uk [P01]

Dalla, Silvia(UniversityofCentralLancashire)sdalla@uclan.ac.uk [P19]

Davidson, Michael(IfA,Edinburgh) mdv@roe.ac.ukDavies, Ben(RochesterInstituteofTechnology,

NY) b.davies@leeds.ac.uk [P02]Davies, Jackie(RutherfordAppletonLaboratory)

jackie.davies@stfc.ac.ukDavies, Roger(UniversityofOxford)

rld@astro.ox.ac.ukDavis, Christopher(STFC RutherfordAppleton

Laboratory) chris.davis@stfc.ac.uk [P24]Davis, Gary(JointAstronomyCentre)

g.davis@jach.hawaii.edu [P05]Davis, Olaf(Oxford) olafdavis@googlemail.com

[P11]Dawson, Ewan(BritishGeologicalSurvey)

ewan@bgs.ac.uk [P18]DeRosa, Robert(UniversityofExeter)

derosa@astro.ex.ac.uk [P32]DePasquale, Massimiliano(UCL/MSSL)

mdp@mssl.ucl.ac.uk [P20]Deane, Roger(Oxford)

roger.deane@astro.ox.ac.uk [P16]DelZanna, Giulio(UniversityofCambridge)

g.del-zanna@damtp.cam.ac.uk [P04]Dere, Ken(GeorgeMasonUniversity)

kdere@gmu.edu [P34]Dickson, Ewan(UniversityofGlasgow)

edickson@astro.gla.ac.uk [P19]Ding, Jiaoyang(ArmaghObservatory)

jyd@arm.ac.uk [P29]Diver, Declan(UniversityofGlasgow)

diver@astro.gla.ac.uk [P30, P29]Dominik, Martin(SUPA,UniversityofStAndrews)

md35@st-andrews.ac.ukDoran, Emile(UniversityofSheffield)

php09eid@sheffield.ac.ukDorrian, Gareth(Queen'sUniversityofBelfast)

g.dorrian@qub.ac.uk [P34]Dougherty, Michele(ImperialCollegeLondon)

m.dougherty@imperial.ac.uk [P09]Down, Emily(UK GeminiSupportGroup)

ejd@astro.ox.ac.uk [P31]Doyle, Gerry(ArmaghObservatory)

jgd@arm.ac.uk [P08]Doyle, Simon(CardiffUNiversity)

simon.doyle@astro.cf.ac.uk [P35]Drake, Alyssa(LJMU) abd@astro.livjm.ac.ukDunlop, James(UniversityofEdinburgh)

jsd@roe.ac.uk [P15]Duthie, Roger(MSSL,UCL) rjad@mssl.ucl.ac.uk

[P03]Eastwood, Jonathan(ImperialCollegeLondon)

jonathan.eastwood@imperial.ac.uk [P03]Efstathiou, George(KavliInstituteforCosmology)

gpe@ast.cam.ac.uk [Plenary]Eldridge, John(InstituteofAstronomy(Cambridge))

jje@ast.cam.ac.uk [P27]Elliott, David(RoyalAstronomicalSociety)

de@ras.org.ukEmerson, Jim(QueenMary, UnivofLondon)

j.p.emerson@qmul.ac.uk [P15]Enoch, Becky(UniversityofStAndrews)

be12@st-andrews.ac.ukErcolano, Barbara(UniversityofExeter)

be@ast.cam.ac.ukEscoubet, C. Philippe(ESA/ESTEC)

philippe.escoubet@esa.int [P03]Espinoza, Cristobal(JodrellBankCentrefor

Astrophysics) cme@jb.man.ac.uk [P30]Evans, Christopher(UK ATC) cje@roe.ac.uk [P02,

P27]Eyres, Stewart(UniversityofCentralLancashire)

spseyres@uclan.ac.ukFalder, James(UniversityofHertfordshire)

J.T.Falder@herts.ac.uk [P31]Fanidakis, Nikolaos(DurhamUniversity)

nikolaos.fanidakis@dur.ac.ukFarihi, Jay(UniversityofLeicester)

jf123@star.le.ac.uk [P12]Fazakerley, Andrew(MSSL-UCL)

anf@mssl.ucl.ac.uk [P03]Fear, Robert(UniversityofLeicester)

r.fear@ion.le.ac.uk [P23]Feix, Martin(UniversityofStAndrews)

mf256@st-andrews.ac.uk [P31, P21, P21]Ferdman, Robert(UniversityofManchester)

robert.ferdman@manchester.ac.uk [P30]Ferreras, Ignacio(MSSL/UCL)

ferreras@star.ucl.ac.uk [P27, P01, P11]Findlay, Joseph(QMUL) j.findlay@qmul.ac.uk

[P15]Fletcher, Lyndsay(UniversityofGlasgow)

Lyndsay@astro.gla.ac.uk [P34, P29, P19,P04, P19, P29]

Fleuren, Simone(QueenMaryUniversityLondon)s.fleuren@qmul.ac.uk

Fludra, Andrzej(STFC RutherfordAppletonLaboratory) andrzej.fludra@stfc.ac.uk [P09,P09]

Forgan, Duncan(SUPA,IfA,UniversityofEdinburgh) dhf@roe.ac.uk [P10]

Forsyth, Colin(UCL MSSL) cfo@mssl.ucl.ac.uk[P03]

Frankland, Victoria(Heriot-WattUniversity)vlf1@hw.ac.uk [P17]

Fraser, HelenJane(SUPA,UniversityofStrathclyde) h.fraser@phys.strath.ac.uk

Fraser, Morgan(QueensUniversityBelfast)mfraser02@qub.ac.uk [P20]

Frenk, Carlos(DurhamUniversity)c.s.frenk@durham.ac.uk [P11]

Fullekrug, Martin(UniversityofBath)eesmf@bath.ac.uk [P18]

Fuller, Gary(JodrellBankCentreforAstrophysics-UK ALMA ARC)G.Fuller@manchester.ac.uk [P17, P02, P17,P17]

Gaensicke, Boris(UniversityofWarwick)Boris.Gaensicke@warwick.ac.uk [P26]

Gallagher, Peter(TrinityCollegeDublin)peter.gallagher@tcd.ie [P24]

Garcia, Percival(Percival&Associates)valgar09@msn.com

Garrett, Michael(ASTRON) dijk@astron.nlGarrington, Simon(UniversityofManchester)

stg@jb.man.ac.uk [P05, P20]Gascoyne, Andrew(UniversityofSheffield)

app07adg@shef.ac.ukGeen, Sam(OxfordAstrophysics)

samgeen@astro.ox.ac.uk [P31]Ghodsi, Hoda(UniversityofGlasgow)

h.ghodsi@astro.gla.ac.uk [P11]Gibson, Brad(UnivofCentralLancashire)

bkgibson@uclan.ac.uk [P31]Gibson, Heather(OpenUniversity)

heg38@student.open.ac.ukGill, Colin(UniversityofGlasgow)

c.gill@astro.gla.ac.ukGilmore, Gerard(InstituteofAstronomy)

gil@ast.cam.ac.ukGonzale-Morales, Pedro-Alejandro(Sheffield

University) pedro.gonzalez@sheffield.ac.ukGoossens, Marcel(K.U.Leuven-CPA)

Marcel.Goossens@wis.kuleuven.beGordon, James(UniversityofCambridge)

jag89@cam.ac.uk [P22]Gordovskyy, Mykola(UniversityofManchester)

mykola.gordovskyy@manchester.ac.uk [P19]Gosling, Andrew(Gemini, Oxford)

ajg@astro.ox.ac.ukGrady, Keith(UniversityofStAndrews)

keithg@mcs.st-andrews.ac.uk [P19, P19]Grady, Monica(TheOpenUniversity)

m.m.grady@open.ac.ukGraham, David(GlasgowUniversity)

d.graham@astro.gla.ac.uk [P04]Granot, Jonathan(UniversityofHertfordshire)

j.granot@herts.ac.uk [P20]Gray, Norman(UniversityofGlasgow)

norman@astro.gla.ac.uk [P10]Green, Lucie(UCL-MSSL) lmg@mssl.ucl.ac.uk

[P09, P33, P04]Gregory, Scott(UniversityofExeter)

scott@astro.ex.ac.uk [P32]Griffin, Matt(CardiffUniversity)

matt.griffin@astro.cf.ac.uk [P07]Grocott, Adrian(UniversityofLeicester)

ag27@ion.le.ac.uk [P18]Guandalini, Roald(UniversityofHertfordshire)

roald_75@yahoo.it [P15]Guo, Jingnan(UniversityofGlasgow)

j.guo@astro.gla.ac.uk [P19]Gupta, Jennifer(JodrellBankCentrefor

Astrophysics)jennifer.gupta@postgrad.manchester.ac.uk[P01]

Gürkan, Gülay(TheUniverstiyofManchester)gulay.gurkan@postgrad.manchester.ac.uk[P21]

Habergham, Stacey(AstrophysicsResearchInstitute) smh@astro.livjm.ac.uk [P02]

Hallinan, Gregg(UC Berkeley)gregg.hallinan@berkeley.edu [P08]

Hambly, Nigel(UniversityofEdinburgh)nch@roe.ac.uk [P10, P15, P10]

98

Hamilton-Morris, Victoria(UniversityofBirmingham) vhh@star.sr.bham.ac.uk [P11]

Hannah, Iain(UniversityofGlasgow)iain@astro.gla.ac.uk [P19, P19, P34, P04]

Hapgood, Mike(STFC RutherfordAppletonLaboratory) mike.hapgood@stfc.ac.uk [P24,P09, P03]

Hargreaves, John(UniversityofLancaster)j.hargreaves@lancaster.ac.uk [P28]

Harra, Louise(UCL-MSSL) lkh@mssl.ucl.ac.uk[P09, P09]

Harris, Jennifer(UniversityofWarwick)j.m.harris@warwick.ac.uk [P34]

Harris, Kathryn(UCLan) kaharris@uclan.ac.uk[P31]

Harrison, Richard(RutherfordAppletonLaboratory) richard.harrison@stfc.ac.uk[P09]

Hatchell, Jennifer(UniversityofExeter)hatchell@astro.ex.ac.uk [Plenary]

Haughian, Karen(UniversityofGlasgow)k.haughian@physics.gla.ac.uk

Hawken, Adam(UCL) ahawken@star.ucl.ac.ukHeavens, Alan(UniversityofEdinburgh)

afh@roe.ac.uk [P21, P21]Hebden, Kerry(JodrellBankCenterfor

Astrophysics)kerry.hebden@postgrad.manchester.ac.uk[P17]

Henault-Brunet, Vincent(InstituteforAstronomy,UniversityofEdinburgh) vhb@roe.ac.uk

Hendry, Martin(UniversityofGlasgow)martin@astro.gla.ac.uk [P11, P33, P33]

Heng, IkSiong(UniversityofGlasgow)i.heng@physics.gla.ac.uk [P30]

Hepburn, Ian(UCL/MSSL) idh@mssl.ucl.ac.uk[P35]

Hermanowicz, Maciej(InstituteofAstronomy,UniversityofCambridge) mth34@cam.ac.uk

Heward, Anita(RoyalAstronomicalSociety)anitaheward@btinternet.com

Heyer, Inge(JointAstronomyCentre)inge_heyer@yahoo.com [P33]

Heymans, Catherine(IfA,UniversityofEdinburgh)heymans@roe.ac.uk [P21]

Higgins, Paul(TrinityCollegeDublin)pohuigin@gmail.com [P34]

Hild, Stefan(UniversityofGlasgow)s.hild@physics.gla.ac.uk [P35]

Hill, David(UniversityofStAndrews)dth4@st-andrews.ac.uk [P01, P01]

Hillier, Dan(RoyalObservatoryEdinburghVisitorCentre) dan.hillier@stfc.ac.uk [P33]

Ho, Wynn(UniversityofSouthampton)wynn.ho@soton.ac.uk [P30]

Holland, Wayne(UK AstronomyTechnologyCentre) wayne.holland@stfc.ac.uk

Holliman, Mark(UniversityofEdinburgh, InstituteforAstronomy) markholliman@gmail.com [P10,P10]

Hood, Alan(UniversityofStAndrews)alan@mcs.st-and.ac.uk [P04]

Hood, Ross(InstituteforAstronomy, UniversityofEdinburgh) rjh@roe.ac.uk

Horn, Markus(ImperialCollegeLondon)m.horn@imperial.ac.uk [P11]

Horne, Keith(SUPA StAndrews)kdh1@st-and.ac.uk

Hornig, Gunnar(UniversityofDundee)gunnar@maths.dundee.ac.uk [P23, P23]

Hough, James(UniversityofHertfordshire)j.h.hough@herts.ac.uk

House, Elisa(UniversityofCentralLancashire)elhouse@uclan.ac.uk [P31]

Hsieh, Henry(QueensUniversityBelfast)h.hsieh@qub.ac.uk [P12]

Huang, Zhenghua(ArmaghObservatory)huangzhenghua@gmail.com [P29]

Hudson, Hugh(SSL/UC Berkeley)hhudson@ssl.berkeley.edu [P29, P14]

Husnoo, Nawal(UniversityofExeter)nawal@astro.ex.ac.uk

Hussain, Gaitee(ESO) ghussain@eso.org [P32]Hutcheon, Richard(KeeleUniversity)

richard.hutcheon@btinternet.com [P27]Hutchinson, James(UniversityofLeicester)

jh251@ion.le.ac.uk [P18]Huxor, Avon(UniversityofBristol)

avon.huxor@bristol.ac.uk [P26, P10]Hyde, Paul(None) g4csd@yahoo.co.ukIbar, Edo(UK AstronomyTechnologyCentre)

ibar@roe.ac.uk [P01]Jain, Rekha(UniversityofSheffield)

R.Jain@sheffield.ac.uk [P23]Jarvis, Matt(UniversityofHertfordshire)

M.J.Jarvis@herts.ac.uk [P31, P15, P06]Jeffries, Rob(KeeleUniversity)

rdj@astro.keele.ac.uk [P32]Jess, David(Queen'sUniversityBelfast)

d.jess@qub.ac.uk [P14, P14, P14]John, Daniel(DurhamUniversity)

d.s.john@durham.ac.uk [P11]Johnson, Olivia(RoyalObservatoryGreenwich)

cocjohnson@googlemail.com [P33]Johnston, Rebecca(UniversityofCambridge)

rrj20@cam.ac.ukJohnston, Russell(UniversityoftheWesternCape)

rwij77@gmail.com [P01]Johnstone, Colin(UniversityofStAndrews)

cpj2@st-andrews.ac.ukJones, Geraint(MSSL,UCL) ghj@mssl.ucl.ac.uk

[P18, P13]Jones, Mark(TheOpenUniversity)

m.h.jones@open.ac.uk [P10]Jones, Olivia(UniversityofManchester)

olivia.jones@postgrad.manchester.ac.uk[P27]

Jonsson, Jakob(UniversityofOxford)jacke@astro.ox.ac.uk [P11]

Jordan, Carole(UniversityofOxford)cj@thphys.ox.ac.uk

Kanani, Sheila(MullardSpaceScienceLaboratory)sk2@mssl.ucl.ac.uk [P18]

Karczewski, Oskar(UCL)o.karczewski.09@ucl.ac.uk

Kaviraj, Sugata(ImperialCollegeLondon)s.kaviraj@imperial.ac.uk [P27]

Kellett, Stephanie(UniversityofLeicester)sk175@ion.le.ac.uk [P18]

Kelly, Gemma(UniversityofLiverpool)G.S.Kelly@liv.ac.uk [P18]

Kelly, James(UCLan) jkelly2@uclan.ac.ukKelvin, Lee(StAndrews) lsk9@st-andrews.ac.uk

[P01, P01]Kennedy, Julia(InstituteforAstronomy, University

ofEdinburgh) jsk@roe.ac.uk [P35]Keogh, Dominic(DurhamUniversity)

d.r.keogh@durham.ac.uk [P30]Kerr, John(None) jrk@hotmail.co.ukKeys, Peter(Queen'sUniversityBelfast)

pkeys02@qub.ac.ukKidd, Robert(LancasterUniversity)

rakidd11@hotmail.com [P13]Kiessling, Alina(UniversityofEdinburgh)

aak@roe.ac.uk [P21]Kim, Hansik(DurhamUniversity)

h.s.kim@durham.ac.uk [P16]King, Robert(UniversityofExeter)

rob@astro.ex.ac.uk [P08]Kipping, David(Harvard-SmithsonianCenterfor

Astrophysics) d.kipping@ucl.ac.uk [P12]Kitching, Thomas(UniversityofEdinburgh)

tdk@roe.ac.ukKiyani, Khurom(UniversityofWarwick)

k.kiyani@warwick.ac.uk [P03]Kofman, Wlodek(LPG CNRS/UJF)

wlodek.kofman@obs.ujf-grenoble.frKontar, Eduard(UniversityofGlasgow)

eduard@astro.gla.ac.uk [P19, P19, P19, P34,P19, P19, P19, P19]

Kukula, Marek(RoyalObservatoryGreenwich)mkukula@nmm.ac.uk [P24, P33]

Kunawicz, Nadya(JodrellBankCentreforAstrophysics) nadya_kunawicz@yahoo.co.uk[P17]

Kurtz, Donald(UniversityofCentralLancashire)dwkurtz@uclan.ac.uk [P33]

Kuznetsov, Alexey(ArmaghObservatory)aku@arm.ac.uk [P08]

Labrosse, Nicolas(UniversityofGlasgow)n.labrosse@physics.gla.ac.uk [P34]

Lacerda, Pedro(Queen'sUniversityBelfast)p.lacerda@qub.ac.uk [P12]

Lacey, Cedric(DurhamUniversity)Cedric.Lacey@durham.ac.uk [P07]

Lang, Pauline(UniversityofStAndrews)pl42@st-andrews.ac.uk [P08]

Lawrence, Andy(UniversityofEdinburgh)al@roe.ac.uk [P16]

Lawrie, Craig(UniversityofGlasgow)c.lawrie@physics.gla.ac.uk [P11]

Lester, Mark(UniversityofLeicester)mle@ion.le.ac.uk [P09, P18]

Levan, Andrew(UniversityofWarwick)A.J.Levan@warwick.ac.uk [P30]

Lewis, Fraser(FaulkesTelescopeProject)lewisf@cf.ac.uk

Lewis, James(InstituteofAstronomy)jrl@ast.cam.ac.uk [P15]

Li, Chuan(MullardSpaceScienceLaboratroy)cl2@mssl.ucl.ac.uk [P19]

Li, Xing(AberystwythUniversity) xxl@aber.ac.uk[P34]

Liang, Guiyun(UniversityofStrathclyde)guiyun.liang@strath.ac.uk [P29]

Liddle, Andrew(UniversityofSussex)a.liddle@sussex.ac.uk

Lin, Bob(Univ.ofCalifornia, Berkeley)rlin@ssl.berkeley.edu [Plenary]

Lintott, Chris(UniversityofOxford)cjl@astro.ox.ac.uk [P24, P10]

Littlefair, Stuart(UniversityofSheffield)s.littlefair@shef.ac.uk [P08]

Liu, Siming(UniversityofGlasgow)sliu@astro.gla.ac.uk [P19, P19]

Loveday, Jon(UniversityofSussex)J.Loveday@sussex.ac.uk [P01, P26]

Lowe, Stuart(TheJodcast)Stuart.Lowe@manchester.ac.uk [P33]

Lowes, Frank(NewcastleUniversity)f.j.lowes@ncl.ac.uk

Lucas, Philip(UniversityofHertfordshire)p.w.lucas@herts.ac.uk [P15]

Lucek, Elizabeth(ImperialCollege)e.lucek@imperial.ac.uk [P03, P09, P09]

Lumsden, Stuart(UniversityofLeeds)s.l.lumsden@leeds.ac.uk

Luna, Marialejandra(UniversityofSheffield)m.luna@sheffield.ac.uk [P14]

Lykou, Foteini(Claire)(JodrellBankCentreforAstrophysics)Foteini.Lykou@postgrad.manchester.ac.uk[P22]

MacKinnon, Alec(UniversityofGlasgow)a.mackinnon@educ.gla.ac.uk [P19, P19, P33]

MacTaggart, David(StAndrews)dm428@st-andrews.ac.uk [P34]

Macdonald, Erin(UniversityofGlasgow)emacdonald@astro.gla.ac.uk [P01]

Mackay, Craig(InstituteofAstronomy, UniversityofCambridge) CDM@ast.cam.ac.uk

Mackay, Duncan(UniversityofStAndrews)duncan@mcs.st-and.ac.uk

Mackay, Mel(InstituteofAstronomy, Universityof

99

Cambridge) mel.mackay@which.netMadjarska, Maria(ArmaghObservatory)

madj@arm.ac.uk [P29, P29]Majewski, Pawel(RutherfordAppletonLaboratory)

pawel.majewski@stfc.ac.uk [P11, P11]Mallik, Procheta(UniversityofGlasgow)

pmallik@astro.gla.ac.uk [P29]Mannering, Elizabeth(UniversityofBristol)

ejamannering@googlemail.com [P31]Marsden, Richard(ESA) Richard.Marsden@esa.int

[P09]Marsh, Mike(UniversityofCentralLancashire)

mike.s.marsh@gmail.com [P14]Mason, Andrew(OpenUniversity)

andym1972@hotmail.com [P02]Mason, Helen(UniversityofCambridge)

hm11@damtp.cam.ac.uk [P33, P04, P34]Massey, Robert(RoyalAstronomicalSociety)

rm@ras.org.ukMassone, AnnaMaria(CNR-SPIN)

annamaria.massone@cnr.it [P10]Masters, Adam(MullardSpaceScience

Laboratory) am2@mssl.ucl.ac.uk [P08]Masters, Richard(OxfordUniversity)

r.masters1@physics.ox.ac.ukMathioudakis, Mihalis(QueensUniversityBelfast)

M.Mathioudakis@qub.ac.uk [P14, P14]Matsuura, Mikako(UniversityCollegeLondon)

mikako@star.ucl.ac.uk [P12]Matthews, Sarah(UCL-MSSL) sam@mssl.ucl.ac.uk

[P04, P23]Mawson, Neil(AstrophysicsResearchInstitute)

nrm@astro.livjm.ac.uk [P05]Maxted, Pierre(KeeleUniversity)

pflm@astro.keele.ac.ukMaxwell, Michael(UCLan)

mpmaxwell@uclan.ac.ukMcCaughrean, Mark(ESA) mjm@esa.int [Plenary]McCombie, June(UniversityofNottingham)

june.mccombie@nottingham.ac.ukMcCoustra, Martin(Heriot-WattUniversity)

m.r.s.mccoustra@hw.ac.uk [P17, P17]McKean, John(ASTRON) mckean@astron.nl [P06]McLauchlan, Rachael(UniversityofGlasgow)

rachael@astro.gla.ac.ukMcLaughlin, James(NorthumbriaUniversity)

james.a.mclaughlin@northumbria.ac.uk[P34]

McMahon, Richard(UniversityofCambridge)rgm@ast.cam.ac.uk [P15]

McQuillin, Rachael(KeeleUniversity)r.c.mcquillin@epsam.keele.ac.uk [P31]

Mecheri, Redouane(QueenMaryUniversityofLondon) r.mecheri@qmul.ac.uk

Melrose, Don(UniversityofSydney)melrose@physics.usyd.edu.au [Plenary]

Meyer, Karen(UniversityofStAndrews)km334@st-andrews.ac.uk [P29]

Meyerdierks, Horst(RoyalObservatoryEdinburgh)hme@roe.ac.uk

Miller, David(UniversityofGlasgow)d.miller@physics.gla.ac.uk [P21]

Miller, Grant(UniversityofStAndrews)gm228@st-andrews.ac.uk [P32]

Miller, Steve(UCL) s.miller@ucl.ac.uk [P13]Mitchell, Cathryn(UniversityofBath)

c.n.mitchell@bath.ac.uk [P18]MitraKraev, Urmila(UniversityofCambridge

(DAMTP)) urmila.mitrakraev@gmail.com[P29]

Moretti, MariaIda(BolognaUniversity)mariaida.moretti@studio.unibo.it [P15]

Morgan, Lawrence(LiverpoolJohnMooresUniversity) lkm@astro.livjm.ac.uk

Morris, Margaret(AstronomicalSocietyofGlasgow) mmorris671@aol.com

Morton, Richard(UniversityofSheffield)app07rjm@shef.ac.uk [P14, P33]

Murphy, David(DurhamUniversity)david.murphy@durham.ac.uk [P26]

Murray, Peter(SUPA InstututeforGravitationalResearch) p.murray@physics.gla.ac.uk

Muxlow, Tom(JodrellBankCentreforAstrophysics) twbm@jb.man.ac.uk [P20, P16]

Nelson, Richard(QueenMary, UniversityofLondon) R.P.Nelson@qmul.ac.uk [Plenary]

Neukirch, Thomas(UniversityofSt.Andrews)thomas@mcs.st-and.ac.uk [P19, P23, P13]

Nicholls, Bella(RoyalAstronomicalSociety)an@ras.org.uk

Nichols, Jonathan(UniversityofLeicester)jdn@ion.le.ac.uk [P08]

Norberg, Peder(IfA,UniversityofEdinburgh)iprn@roe.ac.uk

Norton, Andrew(TheOpenUniversity)a.j.norton@open.ac.uk

Nutter, David(CardiffUniversity)david.nutter@astro.cf.ac.uk [P05]

O'Brien, Paul(UniversityofLeicester)pto@star.le.ac.uk

O'Connor, Terry(STFC) maureen.ayres@stfc.ac.ukO'Dwyer, Brendan(UniversityofCambridge)

bo234@damtp.cam.ac.uk [P34]O'Neil, Robert(UCL MSSL) rho2@mssl.ucl.ac.uk

[P04]O'Regan, Jonathan(MSSL/UCL)

jjo2@mssl.ucl.ac.ukOrza, Beniamin(TheUniversityofSheffield)

app09bo@sheffield.ac.uk [P14]Oudmaijer, Rene(UniversityofLeeds)

r.d.oudmaijer@leeds.ac.uk [P22]Owen, Christopher(UCL/MSSL)

cjo@mssl.ucl.ac.uk [P09]Owens, Mathew(UniversityofReading)

mathewjowens@gmail.com [P24]Owens, Steve(IYA2009)

steve@astronomy2009.co.uk [P33]Parkinson, Hannah(IfA,Edinburgh) hrp@roe.ac.uk

[P01]Parley, Neil(UniversityofStAndrews)

neil.parley@st-andrews.ac.ukParnell, Clare(UniversityofStAndrews)

clare@mcs.st-and.ac.uk [P23]Pascoe, David(UniversityofStAndrews)

dpascoe@mcs.st-and.ac.uk [P14]Pastrav, BogdanAdrian(UCLan)

bapastrav@uclan.ac.ukPatel, Harsit(ImperialCollegeLondon)

hp308@imperial.ac.uk [P07]Patel, Prina(InstitueofCosmology&Gravitation)

prina.patel@port.ac.uk [P06]Patience, Jenny(UniversityofExeter)

patience@astro.ex.ac.uk [P22, P08]Patterson, Brett(UniversityofCentralLancashire)

BAPatterson@uclan.ac.ukPearson, Elizabeth(CardiffUniversity)

Elizabeth.Pearson@astro.cf.ac.ukPedram, Ehsan(UCL MSSL) epe2@mssl.ucl.ac.uk

[P23]Pedretti, Ettore(SUPA,UniversityofStAndrews)

ep41@st-andrews.ac.uk [P22]Penarrubia, Jorge(UniversityofCambridge, IoA)

jorpega@ast.cam.ac.uk [P11]Penny, Alan(U StAndrews)

alan.penny@st-andrews.ac.uk [P06]Percival, Susan(LiverpoolJohnMooresUniversity)

smp@astro.livjm.ac.uk [P27]Phillips, Neil(InstituteforAstronomy, University

ofEdinburgh) nmp@roe.ac.uk [P07]Piana, Michele(Universita'diGenova)

piana@dima.unige.it [P10, P19]Pilkington, Kate(UnivofCentralLancashire)

kpilkington@uclan.ac.uk [P31]Pitkin, Matthew(UniversityofGlasgow)

matthew@astro.gla.ac.uk [P30, P99, P30]Pollacco, Don(QueensUniversityBelfast)

d.pollacco@qub.ac.ukPont, Frederic(UniversityofExeter)

fpont@astro.ex.ac.ukPontin, David(UniversityofDundee)

dpontin@maths.dundee.ac.uk [P23, P23]Popescu, CristinaC. (UCLan)

cpopescu@uclan.ac.uk [P01]Potts, Dale(MullardSpaceScienceLaboratory,

UCL) drp2@mssl.ucl.ac.ukPotts, Hugh(UniversityofGlasgow)

hugh@astro.gla.ac.uk [P29]Predoi, Valeriu(CardiffUniversity)

valeriu.predoi@astro.cf.ac.uk [P20]Prescott, Matthew(LJMU AstrophysicsResearch

Institute) mxp@astro.livjm.ac.uk [P01]Provan, Gabby(UniversityofLeicester)

gp3@ion.le.ac.uk [P18]Quinn, Ciara(CardiffUniversity)

ciara.quinn@astro.cf.ac.ukRahimi, Awat(MSSL (UCL)) ara2@mssl.ucl.ac.uk

[P01]Rainnie, John(RAL) john.rainnie@stfc.ac.ukRamsay, Gavin(ArmaghObservatory)

gar@arm.ac.ukRangel, Cyprian(ImperialCollegeLondon)

cyprian.rangel@imperial.ac.uk [P31]Ratcliffe, Heather(UniversityofGlasgow)

h.ratcliffe@astro.gla.ac.uk [P19]Rawlings, Steve(UniversityofOxford)

vfw@astro.ox.ac.uk [P16, P31, P06]Rea, Alex(UniversityofCambridge)

adr34@mrao.cam.ac.uk [P22]Read, Justin(UniversityofLeicester)

justin.inglis.read@gmail.com [P11]Read, Mike(IfA,UniversityofEdinburgh)

mar@roe.ac.uk [P10, P15, P10]Reay, Sarah(BritishGeologicalSurvey)

sjr@bgs.ac.uk [P18]Regnart, Horace(None) rlo2@tutor.open.ac.ukReid, Hamish(UniversityofGlasgow)

hamish@astro.gla.ac.uk [P19]Richards, Anita(JBCA,UniversityofManchester)

amsr@jb.man.ac.uk [P22, P12]Richer, John(Cambridge) jsr10@cam.ac.uk [P05]Rigby, Emma(UniversityofNottingham)

emma.rigby@nottingham.ac.uk [P07, P16]Rigopoulou, Dimitra(STFC RAL/Oxford)

d.rigopoulou1@physics.ox.ac.uk [P01, P05]Roberts, Bernard(StAndrews)

bernie@mcs.st-and.ac.ukRobertson, David(SheffieldUniversity)

d.robertson@shef.ac.uk [P14]Robotham, Aaron(StAndrews)

asgr@st-andrews.ac.uk [P01, P01, P01]Robson, Ian(UKATC) ian.robson@stfc.ac.ukRoche, Paul(FaulkesTelescopeProject/Cardiff

University)paul.roche@faulkes-telescope.com

Ronald, Kevin(UniversityofStrathclyde)K.Ronald@strath.ac.uk [P13]

Ross, Ashley(UniversityofPortsmouth)ashley.ross@port.ac.uk [P26]

Ross, Nicholas(LawrenceBerkeleyLab)npross@lbl.gov [P26]

Rowlinson, Antonia(UniversityofLeicester)bar7@star.le.ac.uk [P20]

Ruffle, Paul(JodrellBankCentreforAstrophysics)paul@paulruffle.com [P17]

Rushton, Mark(UniversityofCentralLancashire)mrushton@uclan.ac.uk [P02]

Sabiu, Cristiano(None) csabiu@gmail.com [P26]Sakai, Satoru(UniversityofGlasgow)

s.sakai@astro.gla.ac.uk [P30]Salaris, Maurizio(ARI -LiverpoolJohnMoores

University) ms@astro.livjm.ac.ukSantiago, Ignacio(UniversityofGlasgow)

isantiago@physics.gla.ac.ukSathyaprakash, Bangalore(CardiffUniversity)

100

B.Sathyaprakash@astro.cf.ac.uk [Plenary]Selway, Kirsty(UniversityofGlasgow)

pixiequeen10thk@hotmail.co.ukSemionov, Dmitrij(UCLan)

DSemionov@uclan.ac.uk [P01]Senior, Andrew(LancasterUniversity)

a.senior@lancaster.ac.uk [P18]Sharples, Ray(UNIVERSITY OF DURHAM)

R.M.SHARPLES@DURHAM.AC.UK [P05]Sibbons, Lisette(UniversityofHertfordshire)

l.sibbons1@herts.ac.uk [P27]Sibthorpe, Bruce(UK ATC)

bruce.sibthorpe@stfc.ac.uk [P07]Simpson, Chris(LiverpoolJohnMooresUniversity)

cjs@astro.livjm.ac.ukSimpson, Fergus(Edinburgh) frgs@roe.ac.uk [P11]Small, Emma(ARI,LJMU) ees@astro.livjm.ac.ukSmartt, Stephen(Queen'sUniversityBelfast)

s.smartt@qub.ac.ukSmith, Anthony(UniversityofSussex)

anthonysmith80@gmail.com [P07]Smith, Graham(UniversityofBirmingham)

gps@star.sr.bham.ac.ukSmith, Mathew(UCT) mathew.smith@uct.ac.za

[P26]Smith, Matthew(CardiffUniversity)

Matthew.Smith@astro.cf.ac.uk [P07]Smith, P (Wiley-Blackwell) psmith@wiley.comSmith, Rachel(KeeleUniversity)

rs@astro.keele.ac.uk [P22]Smith, Robert(UniversityofSussex)

rcs@sussex.ac.ukSmith, Russell(DurhamUniversity)

russell.smith@durham.ac.uk [P27]Soechting, Ilona(UniversityofOxford)

iks@astro.ox.ac.ukSouthwood, David(ESA)

david.southwood@esa.int [P08]Spain, Timothy(UCL) tim@star.ucl.ac.uk [P18,

P28]Speirs, David(DepartmentofPhysics, University

ofStrathclyde) david.c.speirs@strath.ac.uk[P19]

Squitieri, Valentina(UniversityofBristol)val.squitieri@bris.ac.uk

Stanway, Elizabeth(UniversityofBristol)e.r.stanway@bristol.ac.uk [P27]

Stark, Craig(UniversityofSt.Andrews)craig@mcs.st-and.ac.uk [P19]

Steed, Kimberley(UCL-MSSL) ks3@mssl.ucl.ac.uk[P24]

Steves, Bonnie(GlasgowCaledonianUniversity)B.Steves@gcal.ac.uk [P10]

Stinson, Greg(CentralLancashire)gsstinson@uclan.ac.uk [P31, P31]

Strachan, Mel(UKATC) mel.strachan@stfc.ac.uk[P35]

Stroud, Vanessa(FaulkesTelescopeProject/TheOpenUniversity)vanessa.stroud@faulkes-telescope.com

Subramanian, Srividya(ArmaghObservatory)sri@arm.ac.uk [P24, P29]

Sullivan, Mark(UniversityofOxford)sullivan@astro.ox.ac.uk [P20]

Sun, Jian(UCL-MullardSpaceScienceLaboratory)js2@mssl.ucl.ac.uk [P09]

Sutherland, Will(QueenMary, UniversityofLondon) w.j.sutherland@qmul.ac.uk [P15,P15]

Sutorius, Eckhard(InstituteforAstronomy, ROE)etws@roe.ac.uk [P15, P10]

Tam, Kuan(UniversityofStAndrews)kvt@st-and.ac.uk

Tan, BoonKok(UniversityofOxford)tanbk@astro.ox.ac.uk [P01]

Tanvir, Nial(UniversityofLeicester)nrt3@star.le.ac.uk [Plenary]

Tatton, Bejamin(UniversityofHertfordshire)b.tatton@herts.ac.uk [P27]

Taylor, Matt(EuropeanSpaceAgency)mtaylor@rssd.esa.int [P03]

Taylor, William(RoyalObservatoryEdinburgh)wdt@roe.ac.uk

Thomson, Alan(BritishGeologicalSurvey)awpt@bgs.ac.uk [P18]

Thomson, Edward(UniversityofGlasgow)e.thomson@astro.gla.ac.uk [P11]

Threlfall, James(UniversityofStAndrews)jwt9@st-andrews.ac.uk [P34]

Tillson, Henry(OxfordUniversity)Henry.Tillson@astro.ox.ac.uk

Tinetti, Giovanna(UCL) g.tinetti@ucl.ac.uk[P35]

Tittley, Eric(U ofEdinburgh, ROE) ert@roe.ac.ukTripathi, Durgesh(UniversityofCambridge)

d.tripathi@damtp.cam.ac.uk [P04]Tsiklauri, David(QueenMaryUniversityof

London) D.Tsiklauri@qmul.ac.uk [P29]Tunnicliffe, Rachel(UniversityofWarwick)

r.l.tunnicliffe@warwick.ac.uk [P20]Turkmani, Rim(ImperialCollege)

r.turkmani@ic.ac.uk [P19]Turnbull, Katie(LancasterUniversity)

k.turnbull1@lancaster.ac.uk [P28]VanDoorsselaere, Tom(UniversityofWarwick)

t.van-doorsselaere@warwick.ac.uk [P14]Vanninathan, Kamalam(KamalamVanninathan)

kva@arm.ac.uk [P29]Vardanyan, Mihran(UniversityofOxford)

m.vardanyan1@physics.ox.ac.ukVargasDominguez, Santiago(MSSL/UCL)

svd@mssl.ucl.ac.uk [P04]Verth, Gary(KU Leuven)

gary.verth@wis.kuleuven.be [P14]Vickers, Hannah(UniversityofLeicester)

hmsv1@ion.le.ac.uk [P18]Vidotto, Aline(UniversityofStAndrews)

aav21@st-andrews.ac.uk [P32]Waldmann, Ingo(UCL) ingo@star.ucl.ac.uk

[P12]Walker, Helen(STFC RutherfordAppletonLab)

helen.walker@stfc.ac.uk [P33]Walker, Matthew(InstituteofAstronomy,

UniversityofCambridge)walker@ast.cam.ac.uk [P11]

Walker, Simon(UniversityofWarwick)s.r.walker101@googlemail.com

Wallace, Alison(UCL-MSSL) ajw2@mssl.ucl.ac.uk[P23, P33]

Walsh, Andrew(MSSL-UCL) apw@mssl.ucl.ac.uk[P03]

Walsh, Robert(UniversityofCentralLancashire)rwwalsh@uclan.ac.uk [P09]

Ward-Thompson, Derek(CardiffUniversity)spxdw@astro.cf.ac.uk [P07]

Watson, Fraser(UniversityofGlasgow)f.watson@astro.gla.ac.uk [P34]

Watson, Laura(ImperialCollege, London)

l.watson09@imperial.ac.uk [P25]Weidner, Carsten(UniversityofStAndrews)

cw60@st-andrews.ac.ukWeltevrede, Patrick(JodrellBankCentrefor

Astrophysics)patrick.weltevrede@manchester.ac.uk [P13]

Wesson, Roger(UniversityCollegeLondon)rwesson@star.ucl.ac.uk [P12, P07]

Westmoquette, Mark(UCL) msw@star.ucl.ac.uk[P31]

Whaler, Kathy(UniversityofEdinburgh)kathy.whaler@ed.ac.uk [Plenary]

White, Richard(UniversityofLeeds)r.j.white@leeds.ac.uk [P35]

Wild, Jim(LancasterUniversity)j.wild@lancaster.ac.uk [P18, P33]

Williams, Anthony(UniversityofLeicester)aow2@ion.le.ac.uk [P24, P18]

Williams, David(UCL) drw@mssl.ucl.ac.uk [P09]Wilmot-Smith, Antonia(UniversityofDundee)

antonia@maths.dundee.ac.uk [P23, P23]Wilson, Fiona(UniversityofStAndrews)

fw237@st-andrews.ac.uk [P23]Woan, Graham(UniversityofGlasgow)

graham@astro.gla.ac.uk [P30, P30, P10]Wood, Alan(AberystwythUniversity)

alan.wood@aber.ac.uk [P18, P13]Wood, Patricia(KeeleUniversity)

plw@astro.keele.ac.ukWoodfield, Emma(LancasterUniversity)

Emma.Woodfield@lancaster.ac.uk [P18]Woods, Paul(UniversityofManchester)

paul.woods@manchester.ac.uk [P27]Wright, Andrew(UniversityofStAndrews)

andy@mcs.st-and.ac.uk [P19]Wright, Gillian(UniversityofEdinburgh)

gsw@roe.ac.uk [Plenary]Wu, Xufen(PhysicsandAstronomy, Universityof

StAndrews) xw47@st-andrews.ac.uk [P31]Wyper, Peter(Sheffield)

app09pfw@sheffield.ac.uk [P23]Wyse, Rosie(JohnsHopkinsUniversity)

wyse@pha.jhu.edu [Plenary]Yates, Japheth(UniversityCollegeLondon)

japheth.yates.09@ucl.ac.uk [P08]Yeates, Anthony(UniversityofDundee)

anthony@maths.dundee.ac.uk [P23, P24]Young, John(UniversityofCambridge)

jsy1001@cam.ac.uk [P22, P22, P22]Young, Neil(UniversityofManchester)

neil.young@postgrad.manchester.ac.uk[P30]

Yu, Shenghua(ArmaghObservatory)syu@arm.ac.uk [P08]

Zhang, ZengHua(UniversityofHertfordshire)z.zhang7@herts.ac.uk [P26]

Zhao, Hongsheng(U. ofStAndrews(SUPA))hz4@st-and.ac.uk [P31, P21, P21]

Zharkov, Sergei(MSSL,UCL) sz2@mssl.ucl.ac.uk[P14]

daCosta, AntonioArmando(InstitutoSuperiorTécnico, Lisboa, Portugal)antonio_da_costa@ieee.org [P30]

vanDriel-Gesztelyi, Lidia(MSSL/UCL)lvdg@mssl.ucl.ac.uk [P24, P29]

vanSpaandonk, Lieke(UniversityofWarwick)l.van-spaandonk@warwick.ac.uk [P26]

101

8b9be3970f4d, 2010-04-05T15:25:39+01:00

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