Mathias Th. Keil and Georg G. Raffelt- Monte Carlo Study of Supernova Neutrino Spectra Formation
Georg Raffelt, Max-Planck-Institut für Physik, München25ème Journée Thématique de lIPN, 3 Juin...
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Transcript of Georg Raffelt, Max-Planck-Institut für Physik, München25ème Journée Thématique de lIPN, 3 Juin...
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
SN 1006SN 1006
Georg Raffelt, Max-Planck-Institut für Physik, Georg Raffelt, Max-Planck-Institut für Physik, MünchenMünchen
2525èmeème Journée Thématique de l’IPN, 3 Juin 2008, Orsay Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Frontiers ofFrontiers ofLow-Energy Neutrino Astronomy:Low-Energy Neutrino Astronomy:Earth, Sun and SupernovaeEarth, Sun and Supernovae
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Where do Neutrinos Appear in Nature?Where do Neutrinos Appear in Nature?
AstrophysicalAstrophysicalAccelerators Accelerators Soon ?Soon ?
Cosmic Big Bang Cosmic Big Bang (Today 330 (Today 330 /cm/cm33)) Indirect EvidenceIndirect Evidence
Nuclear ReactorsNuclear Reactors
Particle AcceleratorsParticle Accelerators
Earth AtmosphereEarth Atmosphere(Cosmic Rays)(Cosmic Rays)
SunSun
SupernovaeSupernovae(Stellar Collapse)(Stellar Collapse)
SN 1987ASN 1987A
Earth Crust Earth Crust (Natural (Natural Radioactivity)Radioactivity)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Neutrinos from nuclearNeutrinos from nuclearreactions:reactions:
Energies 1Energies 120 MeV20 MeV
““Beam dump neutrinos”Beam dump neutrinos”• High-energy protons hitHigh-energy protons hit matter or photonsmatter or photons
• Produce secondary Produce secondary
• Neutrinos from pionNeutrinos from pion decay decay
ee ee
• Energies Energies ≫≫ GeV GeV
Quasi thermal sourcesQuasi thermal sources
Supernova: T ~ few MeVSupernova: T ~ few MeV
Big-Bang Neutrinos:Big-Bang Neutrinos:Very small energies todayVery small energies today(cosmic red shift)(cosmic red shift)
Like matter todayLike matter today
Where do Neutrinos Appear in Nature?Where do Neutrinos Appear in Nature?
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Low-energyLow-energyneutrino astronomyneutrino astronomy(including geo-neutrinos)(including geo-neutrinos)Energies ~ 1Energies ~ 150 MeV50 MeV
High-energyHigh-energyneutrino astronomyneutrino astronomy
Closely related toClosely related tocosmic-ray physicscosmic-ray physics
Long-baselineLong-baselineneutrino oscillationneutrino oscillationexperiments withexperiments with• Reactor neutrinosReactor neutrinos• Neutrino beams fromNeutrino beams from acceleratorsaccelerators
Where do Neutrinos Appear in Nature?Where do Neutrinos Appear in Nature?
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Hans Bethe (1906Hans Bethe (19062005, Nobel prize 1967)2005, Nobel prize 1967)Thermonuclear reaction chains (1938)Thermonuclear reaction chains (1938)
Neutrinos from the SunNeutrinos from the Sun
Solar radiation: 98 % lightSolar radiation: 98 % light 2 % neutrinos2 % neutrinosAt Earth 66 billion neutrinos/cmAt Earth 66 billion neutrinos/cm22 sec sec
Reaction-Reaction-chainschains
EnergyEnergy26.7 MeV26.7 MeV
HeliumHelium
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Bethe’s Classic Paper on Nuclear Reactions in Bethe’s Classic Paper on Nuclear Reactions in StarsStars
No neutrinosNo neutrinosfrom nuclear from nuclear
reactionsreactionsin 1938 … in 1938 …
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Gamow & Schoenberg, Phys. Rev. 58:1117 Gamow & Schoenberg, Phys. Rev. 58:1117 (1940)(1940)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Sun Glasses for Neutrinos?Sun Glasses for Neutrinos?
Several light years of lead Several light years of lead needed to shield solarneeded to shield solar neutrinosneutrinos
Bethe & Peierls 1934:Bethe & Peierls 1934: “… “… this evidently meansthis evidently means that one will never be ablethat one will never be able to observe a neutrino.”to observe a neutrino.”
8.3 light minutes8.3 light minutes
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
First Detection (1954 -First Detection (1954 - 1956)1956)
Fred ReinesFred Reines(1918 – 1998)(1918 – 1998)
Nobel prize 1995Nobel prize 1995
Clyde CowanClyde Cowan(1919 – 1974)(1919 – 1974)
Detector prototypeDetector prototype
Anti-Electron Anti-Electron NeutrinosNeutrinosfrom from Hanford Hanford Nuclear ReactorNuclear Reactor
3 Gammas3 Gammasin coincidencein coincidenceee pppp
nnnn CdCdCdCd
ee++ee++ ee--ee--
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Inverse beta decayInverse beta decayof chlorineof chlorine
600 tons of600 tons ofPerchloroethylenePerchloroethylene
Homestake solar neutrinoHomestake solar neutrino observatory (1967observatory (19672002)2002)
First Measurement of Solar NeutrinosFirst Measurement of Solar Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Cherenkov EffectCherenkov EffectCherenkov EffectCherenkov Effect
WaterWater
Elastic Elastic scattering or CC scattering or CC
reactionreaction
Neutrino
NeutrinoLightLight
LightLight
CherenkCherenkov Ringov Ring
Electron or MuonElectron or Muon(Charged Particle)(Charged Particle)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Super-Kamiokande: Sun in the Light of Super-Kamiokande: Sun in the Light of NeutrinosNeutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
2002 Physics Nobel Prize for Neutrino 2002 Physics Nobel Prize for Neutrino AstronomyAstronomy
Ray Davis Jr.Ray Davis Jr.(1914 (1914 2006)2006)
Masatoshi KoshibaMasatoshi Koshiba(*1926)(*1926)
““for pioneering contributions to astrophysics, in for pioneering contributions to astrophysics, in particular for the detection of cosmic neutrinos”particular for the detection of cosmic neutrinos”
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
John BahcallJohn Bahcall1934 1934 20052005
Raymond Davis Jr.Raymond Davis Jr.1914 1914 2006 2006
Missing Neutrinos from the SunMissing Neutrinos from the Sun
HomestakeHomestake
ChlorineChlorine
77BeBe
88BB
CNOCNO
Measurement (1970Measurement (1970 –– 1995)1995)
Calculation of expectedCalculation of expectedexperimental countingexperimental countingrate from variousrate from varioussource reactionssource reactions
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Neutrino Flavor OscillationsNeutrino Flavor Oscillations
Two-flavor mixingTwo-flavor mixing
2
1e
cossin
sincos
2
1e
cossin
sincos
Bruno PontecorvoBruno Pontecorvo(1913 – 1993)(1913 – 1993)
Invented nu oscillationsInvented nu oscillations
Each mass eigenstate propagates asEach mass eigenstate propagates as
with with
ipzeipze
E2m
EmEp2
22 E2
mEmEp
222
zE2
m2z
E2m2
Phase difference implies flavor oscillationsPhase difference implies flavor oscillations
Oscillation Oscillation LengthLength
2
2
2 m
eVMeVE
m5.2m
E4
2
2
2 m
eVMeVE
m5.2m
E4
sinsin22(2(2))
ProbabilityProbability ee
zz
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Missing Neutrinos from the SunMissing Neutrinos from the Sun
HomestakeHomestake
77BeBe
88BB
CNOCNO
ChlorineChlorine
Gallex/GNOGallex/GNOSAGESAGE
CNOCNO
77BeBe
pppp
88BB
GalliumGallium
Electron-Neutrino DetectorsElectron-Neutrino Detectors
(Super-)(Super-)KamiokandeKamiokande
88BB
WaterWateree++ ee ee++ ee
SNOSNO
88BB
ee++ dd pp ++ pp ++ eeHeavy WaterHeavy Water
88BB
++ dd pp ++ nn ++ Heavy WaterHeavy Water
All FlavorsAll Flavors
SNOSNO
88BB
WaterWater + e+ e + e+ e
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Three-Flavor Neutrino ParametersThree-Flavor Neutrino Parameters
3
2
1
1212
1212
1313
1313
2323
2323
e
1
CS
SC
CS
1
SC
CS
SC
1
3
2
1
1212
1212
1313
1313
2323
2323
e
1
CS
SC
CS
1
SC
CS
SC
1 ie ie
ie ie
.,etccosC 1212 .,etccosC 1212 CP-violating phaseCP-violating phase
SolarSolar75759292
AtmosphericAtmospheric1400140030003000
22 meVm 22 meVm
CHOOZCHOOZ Solar/KamLANDSolar/KamLAND 22 ranges rangeshep-ph/0405172hep-ph/0405172
Atmospheric/K2KAtmospheric/K2K 5437 23 5437 23 1113 1113 3630 12 3630 12
ee
ee
11SunSun
NormalNormal
22
33
AtmosphereAtmosphere
ee
ee
11SunSun
InvertedInverted22
33
AtmosphereAtmosphere
Tasks and Open QuestionsTasks and Open Questions
• Precision for Precision for 12 12 andand 2323
• How large is How large is 1313 ??
• CP-violating phase CP-violating phase ??• Mass orderingMass ordering ? ? (normal vs inverted)(normal vs inverted)• Absolute massesAbsolute masses ?? (hierarchical vs degenerate)(hierarchical vs degenerate)• Dirac or MajoranaDirac or Majorana ??
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Solar Neutrino SpectrumSolar Neutrino Spectrum
7-Be line measured7-Be line measuredby Borexino (2007)by Borexino (2007)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Solar Neutrino Spectroscopy with Solar Neutrino Spectroscopy with BOREXINOBOREXINO
• Neutrino electron scatteringNeutrino electron scattering• Liquid scintillator technologyLiquid scintillator technology (~ 300 tons)(~ 300 tons)• Low energy thresholdLow energy threshold (~ 60 keV)(~ 60 keV)• Online since 16 May 2007Online since 16 May 2007
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
• Expected without flavor Expected without flavor oscillationsoscillations75 75 ± 4 ± 4 counts/100t/dcounts/100t/d
• Expected with oscillationsExpected with oscillations49 ± 4 49 ± 4 counts/100t/dcounts/100t/d
• BOREXINO result (May BOREXINO result (May 2008)2008)
49 ± 349 ± 3statstat ± 4 ± 4syssys cnts/100t/dcnts/100t/d arXiv:0805.3843 (25 May 2008)arXiv:0805.3843 (25 May 2008)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Next Steps in BorexinoNext Steps in Borexino
• Collect more statistics of Beryllium lineCollect more statistics of Beryllium line
• Seasonal variation of rateSeasonal variation of rate (Earth orbit eccentricity)(Earth orbit eccentricity)
• Measure neutrinos from the CNO reaction chainMeasure neutrinos from the CNO reaction chain• Information about solar metal abundanceInformation about solar metal abundance
Measure geo-neutrinos Measure geo-neutrinos (from natural radioactivity in the Earth crust)(from natural radioactivity in the Earth crust) Approx. 7Approx. 717 events/year17 events/year Main background: Reactors ~ 20 events/yearMain background: Reactors ~ 20 events/year
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Geo Neutrinos: Why and What?Geo Neutrinos: Why and What?
We know surprisingly little aboutWe know surprisingly little aboutthe interior of the Earth:the interior of the Earth:
• Deepest bore hole ~ 12 kmDeepest bore hole ~ 12 km• Samples from the crust areSamples from the crust are available for chemical analysisavailable for chemical analysis (e.g. vulcanoes)(e.g. vulcanoes)• Seismology reconstructs densitySeismology reconstructs density profile throughout the Earthprofile throughout the Earth• Heat flow from measuredHeat flow from measured temperature gradients 30temperature gradients 3044 TW44 TW (BSE canonical model, based on(BSE canonical model, based on cosmochemical arguments,cosmochemical arguments, predicts ~ 19 TW from crust and predicts ~ 19 TW from crust and mantle, none from core)mantle, none from core)
• Neutrinos escape freelyNeutrinos escape freely
• Carry information about chemical composition, radioactive heat production,Carry information about chemical composition, radioactive heat production, or even a putative natural reactor at the coreor even a putative natural reactor at the core
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Expected Geo Neutrino FluxesExpected Geo Neutrino Fluxes
S. Dye, Talk 5/25/2006S. Dye, Talk 5/25/2006BaltimoreBaltimore
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Geo NeutrinosGeo Neutrinos
Predicted geo neutrino fluxPredicted geo neutrino flux
Reactor backgroundReactor background
KamLAND scintillator detector (1 kton)KamLAND scintillator detector (1 kton)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Kamland Observation of GeoneutrinosKamland Observation of Geoneutrinos
• First tentative observation of geoneutrinosFirst tentative observation of geoneutrinos at Kamland in 2005 (~ 2 sigma effect)at Kamland in 2005 (~ 2 sigma effect)• Very difficult because of large backgroundVery difficult because of large background of reactor neutrinosof reactor neutrinos (is main purpose for neutrino oscillations)(is main purpose for neutrino oscillations)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Sanduleak Sanduleak 69 69 202202
Large Magellanic Cloud Large Magellanic Cloud Distance 50 kpcDistance 50 kpc (160.000 light years)(160.000 light years)
Tarantula NebulaTarantula Nebula
Supernova 1987ASupernova 1987A 23 February 198723 February 1987
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Helium-burning starHelium-burning star
HeliumHeliumBurningBurning
HydrogenHydrogenBurningBurning
Main-sequence starMain-sequence star
Hydrogen BurningHydrogen Burning
Onion structureOnion structure
Degenerate iron core:Degenerate iron core: 101099 g cm g cm33
T T 10 1010 10 K K
MMFeFe 1.5 M 1.5 Msunsun
RRFeFe 8000 km 8000 km
Collapse (implosion)Collapse (implosion)
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Collapse (implosion)Collapse (implosion)ExplosionExplosionNewborn Neutron StarNewborn Neutron Star
~ 50 km~ 50 km
Proto-Neutron StarProto-Neutron Star
nucnuc 3 3 10101414 g cm g cm33
T T 30 MeV 30 MeV
NeutrinoNeutrinoCoolingCooling
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Newborn Neutron StarNewborn Neutron Star
~ 50 km~ 50 km
Proto-Neutron StarProto-Neutron Star
nucnuc 3 3 10101414 g cm g cm33
T T 30 MeV 30 MeV
NeutrinoNeutrinoCoolingCooling
Gravitational binding energyGravitational binding energy
EEbb 3 3 10 105353 erg erg 17% M 17% MSUN SUN cc22
This shows up as This shows up as 99% Neutrinos99% Neutrinos 1% Kinetic energy of explosion1% Kinetic energy of explosion (1% of this into cosmic rays) (1% of this into cosmic rays) 0.01% Photons, outshine host galaxy0.01% Photons, outshine host galaxy
Neutrino luminosityNeutrino luminosity
LL 3 3 10 105353 erg / 3 sec erg / 3 sec
3 3 10 101919 L LSUNSUN
While it lasts, outshines the entireWhile it lasts, outshines the entire visible universevisible universe
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Neutrino Signal of Supernova 1987ANeutrino Signal of Supernova 1987A
Within clock uncertainties,Within clock uncertainties,signals are contemporaneoussignals are contemporaneous
Kamiokande-II (Japan)Kamiokande-II (Japan)Water Cherenkov detectorWater Cherenkov detector2140 tons2140 tonsClock uncertainty Clock uncertainty 1 min1 min
Irvine-Michigan-Brookhaven (US)Irvine-Michigan-Brookhaven (US)Water Cherenkov detectorWater Cherenkov detector6800 tons6800 tonsClock uncertainty Clock uncertainty 50 ms50 ms
Baksan Scintillator TelescopeBaksan Scintillator Telescope(Soviet Union), 200 tons(Soviet Union), 200 tonsRandom event cluster ~ 0.7/dayRandom event cluster ~ 0.7/dayClock uncertainty +2/-54 sClock uncertainty +2/-54 s
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
The Energy-Loss ArgumentThe Energy-Loss Argument
NeutrinoNeutrinospheresphere
NeutrinoNeutrino diffusiondiffusion
Late-time signal most sensitive observableLate-time signal most sensitive observable
Emission of very weakly interactingEmission of very weakly interactingparticles would “steal” energy from theparticles would “steal” energy from theneutrino burst and shorten it.neutrino burst and shorten it.(Early neutrino burst powered by accretion,(Early neutrino burst powered by accretion, not sensitive to volume energy loss.)not sensitive to volume energy loss.)
Volume emissionVolume emission of novel particlesof novel particles
SN 1987A neutrino signalSN 1987A neutrino signal
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Do Neutrinos Gravitate?Do Neutrinos Gravitate?
Neutrinos arrive a few hours earlier than photons Neutrinos arrive a few hours earlier than photons Early warning (SNEWS) Early warning (SNEWS)SN 1987A: Transit time for photons and neutrinos equal to within ~ 3hSN 1987A: Transit time for photons and neutrinos equal to within ~ 3h
Equal within ~ 1 Equal within ~ 1 4 4 101033
Shapiro time delay for particles moving in a Shapiro time delay for particles moving in a gravitational potential gravitational potential
Longo, PRL 60:173,1988Longo, PRL 60:173,1988Krauss & Tremaine, PRL 60:176,1988Krauss & Tremaine, PRL 60:176,1988
• Proves directly that neutrinos respond to gravity in the usual wayProves directly that neutrinos respond to gravity in the usual way because for photons gravitational lensing already proves this pointbecause for photons gravitational lensing already proves this point
• Cosmological limits Cosmological limits NN ≲≲ 1 much worse test of neutrino gravitation 1 much worse test of neutrino gravitation
• Provides limits on parameters of certain non-GR theories of gravitationProvides limits on parameters of certain non-GR theories of gravitation
months51dt)]t(r[U2t BAShapiro months51dt)]t(r[U2t BAShapiro
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Neutrino-Driven Delayed ExplosionNeutrino-Driven Delayed Explosion
Picture adapted from Janka, astro-ph/0008432Picture adapted from Janka, astro-ph/0008432
Neutrino heatingNeutrino heatingincreases pressureincreases pressurebehind shock frontbehind shock front
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Standing Accretion Shock Instability (SASI)Standing Accretion Shock Instability (SASI)Mezzacappa et al., http://www.phy.ornl.gov/tsi/pages/simulations.htmlMezzacappa et al., http://www.phy.ornl.gov/tsi/pages/simulations.html
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Large Detectors for Supernova NeutrinosLarge Detectors for Supernova Neutrinos
Super-Kamiokande (10Super-Kamiokande (1044))KamLAND (400)KamLAND (400)
MiniBooNEMiniBooNE(200)(200)
In brackets eventsIn brackets eventsfor a “fiducial SN”for a “fiducial SN”at distance 10 kpcat distance 10 kpc
LVD (400)LVD (400)Borexino (100)Borexino (100)
IceCube (10IceCube (1066))
BaksanBaksan (100)(100)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Simulated Supernova Signal at Super-Simulated Supernova Signal at Super-KamiokandeKamiokande
Simulation for Super-Kamiokande SN signal at 10 kpc,Simulation for Super-Kamiokande SN signal at 10 kpc,based on a numerical Livermore modelbased on a numerical Livermore model
[Totani, Sato, Dalhed & Wilson, ApJ 496 (1998) 216][Totani, Sato, Dalhed & Wilson, ApJ 496 (1998) 216]
AccretioAccretionn
PhasePhase
Kelvin-Kelvin-HelmholtzHelmholtz
Cooling PhaseCooling Phase
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
IceCube Neutrino Telescope at the South PoleIceCube Neutrino Telescope at the South Pole
• 1 km1 km33 antarctic ice, instrumented antarctic ice, instrumented with 4800 photomultiplierswith 4800 photomultipliers• 40 of 80 strings installed (2008)40 of 80 strings installed (2008)• Completion until 2011 foreseenCompletion until 2011 foreseen
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
IceCube as a Supernova Neutrino DetectorIceCube as a Supernova Neutrino Detector
Each optical module (OM) picks upEach optical module (OM) picks upCherenkov light from its neighborhood.Cherenkov light from its neighborhood.SN appears as “correlated noise”.SN appears as “correlated noise”.
• About 300About 300 CherenkovCherenkov photons photons per OMper OM from a SNfrom a SN at 10 kpcat 10 kpc
• NoiseNoise per OMper OM < 260 Hz< 260 Hz
• Total ofTotal of 4800 OMs4800 OMs in IceCubein IceCube
IceCube SN signal at 10 kpc, basedIceCube SN signal at 10 kpc, basedon a numerical Livermore modelon a numerical Livermore model[Dighe, Keil & Raffelt, hep-ph/0303210][Dighe, Keil & Raffelt, hep-ph/0303210]
Method first discussed byMethod first discussed by• Pryor, Roos & Webster,Pryor, Roos & Webster, ApJ 329:355 (1988)ApJ 329:355 (1988)• Halzen, Jacobsen & ZasHalzen, Jacobsen & Zas astro-ph/9512080astro-ph/9512080
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Neutrino Oscillations in MatterNeutrino Oscillations in Matter
• “ “Level crossing” possible in a medium with a gradient (MSW effect)Level crossing” possible in a medium with a gradient (MSW effect) - For solar nus large flavor conversion anyway due to large mixing- For solar nus large flavor conversion anyway due to large mixing - Still important for 13-oscillations in supernova envelope- Still important for 13-oscillations in supernova envelope• Breaks degeneracy between Breaks degeneracy between and and /2 /2 (dark vs light side) (dark vs light side) - 12 mass ordering for solar nus established- 12 mass ordering for solar nus established - 13 mass ordering (normal vs inverted) at future LBL or SN- 13 mass ordering (normal vs inverted) at future LBL or SN• Discriminates against sterile nus in atmospheric oscillationsDiscriminates against sterile nus in atmospheric oscillations• CP asymmetry in LBL, to be distinguished from intrinsic CP violationCP asymmetry in LBL, to be distinguished from intrinsic CP violation• Prevents flavor conversion in a SN core and within shock wavePrevents flavor conversion in a SN core and within shock wave• Strongly affects sterile nu production in SN or early universeStrongly affects sterile nu production in SN or early universe
Lincoln WolfensteinLincoln Wolfenstein
ff
ZZ
W, ZW, Z
ff
Neutrinos in a medium suffer flavor-dependentNeutrinos in a medium suffer flavor-dependentrefraction (PRD 17:2369, 1978)refraction (PRD 17:2369, 1978)
e
n21
n21
eF
2e
n0
0nnG2
E2M
zi
e
n21
n21
eF
2e
n0
0nnG2
E2M
zi
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
H- and L-Resonance for MSW OscillationsH- and L-Resonance for MSW Oscillations
R. Tomàs, M. Kachelriess,R. Tomàs, M. Kachelriess,G. Raffelt, A. Dighe,G. Raffelt, A. Dighe,H.-T. Janka & L. Scheck: H.-T. Janka & L. Scheck: Neutrino signatures ofNeutrino signatures ofsupernova forward andsupernova forward andreverse shock propagationreverse shock propagation[astro-ph/0407132] [astro-ph/0407132]
ResonancResonanceedensity density forfor
2atmm 2atmm
ResonancResonanceedensity density forfor
2solm 2solm
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Shock-Wave Propagation in IceCubeShock-Wave Propagation in IceCube
Choubey, Harries & Ross, “Probing neutrino oscillations from supernovae shockChoubey, Harries & Ross, “Probing neutrino oscillations from supernovae shockwaves via the IceCube detector”, astro-ph/0604300waves via the IceCube detector”, astro-ph/0604300
Normal HierarchyNormal Hierarchy
Inverted HierarchyInverted HierarchyNo shockwaveNo shockwave
Inverted HierarchyInverted HierarchyForward shockForward shock
Inverted HierarchyInverted HierarchyForward & reverse shockForward & reverse shock
,8.0)(Flux)(Flux
x
e
,8.0)(Flux)(Flux
x
e
MeV18E,MeV15Exe
MeV18E,MeV15Exe
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Collective Effects in Neutrino Flavor Collective Effects in Neutrino Flavor OscillationsOscillationsCollapsed supernova core or accretion torus ofCollapsed supernova core or accretion torus ofmerging neutron stars:merging neutron stars:
• Neutrino flux very dense: Up to 10Neutrino flux very dense: Up to 103535 cm cm3 3
• Neutrino-neutrino interaction energy Neutrino-neutrino interaction energy much larger than vacuum oscillation frequencymuch larger than vacuum oscillation frequency• Large “matter effect” of neutrinos on eachLarge “matter effect” of neutrinos on each otherother• Non-linear oscillation effectsNon-linear oscillation effects
• Assume 80% anti-neutrinosAssume 80% anti-neutrinos• Vacuum oscillation frequencyVacuum oscillation frequency
= 0.3 km= 0.3 km11
• Neutrino-neutrino interaction Neutrino-neutrino interaction energy at nu sphere (r = 10 km)energy at nu sphere (r = 10 km)
= 0.3= 0.3101055 km km11
• Falls off approximately as Falls off approximately as rr44
(geometric flux dilution and nus(geometric flux dilution and nus become more co-linear)become more co-linear)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Spectral Split (Stepwise Spectral Swapping)Spectral Split (Stepwise Spectral Swapping)
Fogli, Lisi, Marrone & Mirizzi, arXiv:0707.1998Fogli, Lisi, Marrone & Mirizzi, arXiv:0707.1998
Initial fluxesInitial fluxesat nu sphereat nu sphere
AfterAftercollectivecollectivetrans-trans-formationformation
For explanation seeFor explanation see
Raffelt & SmirnovRaffelt & Smirnov arXiv:0705.1830arXiv:0705.1830 arXiv:0709.4641arXiv:0709.4641
Duan, Fuller,Duan, Fuller,Carlson & QianCarlson & Qian arXiv:0706.4293arXiv:0706.4293 arXiv:0707.0290arXiv:0707.0290
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Mass Hierarchy at Extremely Small Theta-13Mass Hierarchy at Extremely Small Theta-13
Dasgupta, Dighe & Mirizzi, arXiv:0802.1481Dasgupta, Dighe & Mirizzi, arXiv:0802.1481
Ratio of spectra inRatio of spectra intwo water Cherenkovtwo water Cherenkovdetectors (0.4 Mton),detectors (0.4 Mton),one shadowed by theone shadowed by theEarth, the other notEarth, the other not
Using Earth matter effects to diagnose transformationsUsing Earth matter effects to diagnose transformations
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Collective SN neutrino oscillations 2006-2008 Collective SN neutrino oscillations 2006-2008 (I)(I)
““Bipolar” collective transformationsBipolar” collective transformationsimportant, even for dense matterimportant, even for dense matter
• Duan, Fuller & Qian Duan, Fuller & Qian astro-ph/0511275astro-ph/0511275
Numerical simulationsNumerical simulations• Including multi-angle effectsIncluding multi-angle effects• Discovery of “spectral splits”Discovery of “spectral splits”
• Duan, Fuller, Carlson & QianDuan, Fuller, Carlson & Qian astro-ph/0606616, 0608050astro-ph/0606616, 0608050
• Pendulum in flavor spacePendulum in flavor space• Collective pair annihilationCollective pair annihilation• Pure precession modePure precession mode
• Hannestad, Raffelt, Sigl & WongHannestad, Raffelt, Sigl & Wong astro-ph/0608695astro-ph/0608695• Duan, Fuller, Carlson & QianDuan, Fuller, Carlson & Qian astro-ph/0703776astro-ph/0703776
Self-maintained coherenceSelf-maintained coherencevs. self-induced decoherencevs. self-induced decoherencecaused by multi-angle effectscaused by multi-angle effects
• Sawyer, hep-ph/0408265, 0503013 Sawyer, hep-ph/0408265, 0503013 • Raffelt & Sigl, hep-ph/0701182Raffelt & Sigl, hep-ph/0701182• Esteban-Pretel, Pastor, Tomàs,Esteban-Pretel, Pastor, Tomàs, Raffelt & Sigl, arXiv:0706.2498Raffelt & Sigl, arXiv:0706.2498
Theory of “spectral splits”Theory of “spectral splits”in terms of adiabatic evolution inin terms of adiabatic evolution inrotating framerotating frame
• Raffelt & Smirnov,Raffelt & Smirnov, arXiv:0705.1830, 0709.4641 arXiv:0705.1830, 0709.4641 • Duan, Fuller, Carlson & QianDuan, Fuller, Carlson & Qian arXiv:0706.4293, 0707.0290 arXiv:0706.4293, 0707.0290
Independent numerical simulationsIndependent numerical simulations • Fogli, Lisi, Marrone & MirizziFogli, Lisi, Marrone & Mirizzi arXiv:0707.1998 arXiv:0707.1998
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Collective SN neutrino oscillations 2006-2008 Collective SN neutrino oscillations 2006-2008 (II)(II)
Second-order mu-tau refractive effectSecond-order mu-tau refractive effectimportant in three-flavor contextimportant in three-flavor context
• Esteban-Pretel, Pastor, Tomàs,Esteban-Pretel, Pastor, Tomàs, Raffelt & Sigl, arXiv:0712.1137Raffelt & Sigl, arXiv:0712.1137
Three-flavor effects in O-Ne-Mg SNeThree-flavor effects in O-Ne-Mg SNeon neutronization burston neutronization burst(MSW-prepared spectral double split)(MSW-prepared spectral double split)
• Duan, Fuller, Carlson & Qian,Duan, Fuller, Carlson & Qian, arXiv:0710.1271arXiv:0710.1271• Dasgupta, Dighe, Mirrizzi & Raffelt,Dasgupta, Dighe, Mirrizzi & Raffelt, arXiv:0801.1660arXiv:0801.1660
Theory of three-flavor collectiveTheory of three-flavor collectiveoscillationsoscillations
• Dasgupta & Dighe,Dasgupta & Dighe, arXiv:0712.3798arXiv:0712.3798
Identifying the neutrino mass hierarchyIdentifying the neutrino mass hierarchyat extremely small Theta-13at extremely small Theta-13
• Dasgupta, Dighe & Mirizzi,Dasgupta, Dighe & Mirizzi, arXiv:0802.1481arXiv:0802.1481
Formulation for non-sphericalFormulation for non-sphericalgeometrygeometry
• Dasgupta, Dighe, Mirizzi & RaffeltDasgupta, Dighe, Mirizzi & Raffelt arXiv:0805.3300arXiv:0805.3300
Many theoretical questions for this neutrino many-body systemMany theoretical questions for this neutrino many-body systemremain unresolvedremain unresolved !!
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Core-Collapse SN Rate in the Milky WayCore-Collapse SN Rate in the Milky Way
Gamma rays fromGamma rays from2626Al (Milky Way)Al (Milky Way)
Historical galacticHistorical galacticSNe (all types)SNe (all types)
SN statistics inSN statistics inexternal galaxiesexternal galaxies
No galacticNo galacticneutrino burstneutrino burst
Core-collapse SNe per centuryCore-collapse SNe per century00 11 22 33 44 55 66 77 88 99 1010
van den Bergh & McClure (1994)van den Bergh & McClure (1994)
Cappellaro & Turatto (2000)Cappellaro & Turatto (2000)
Diehl et al. (2006)Diehl et al. (2006)
Tammann et al. (1994)Tammann et al. (1994)Strom (1994)Strom (1994)
90 90 %% CL (25 y obserservation) CL (25 y obserservation) Alekseev et al. (1993)Alekseev et al. (1993)
References: van den Bergh & McClure, ApJ 425 (1994) 205. Cappellaro & References: van den Bergh & McClure, ApJ 425 (1994) 205. Cappellaro & Turatto, astro-ph/0012455. Diehl et al., Nature 439 (2006) 45. Strom, Astron. Turatto, astro-ph/0012455. Diehl et al., Nature 439 (2006) 45. Strom, Astron. Astrophys. 288 (1994) L1. Tammann et al., ApJ 92 (1994) 487. Alekeseev et al., Astrophys. 288 (1994) L1. Tammann et al., ApJ 92 (1994) 487. Alekeseev et al., JETP 77 (1993) 339 and my update.JETP 77 (1993) 339 and my update.
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
SSuperuperNNova ova EEarly arly WWarning arning SSystem (SNEWS)ystem (SNEWS)
Neutrino observation can alert astronomersNeutrino observation can alert astronomersseveral hours in advance to a supernova.several hours in advance to a supernova.To avoid false alarms, require alarm from atTo avoid false alarms, require alarm from atleast two experiments.least two experiments.
CoincidenceCoincidenceServer Server @ BNL@ BNL
Super-KSuper-K
AlertAlert
Others ?Others ?
LVDLVD
IceCubeIceCube
http://snews.bnl.govhttp://snews.bnl.govastro-ph/0406214astro-ph/0406214
Supernova 1987ASupernova 1987AEarly Light CurveEarly Light Curve
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
Experimental Limits on Relic Supernova Experimental Limits on Relic Supernova NeutrinosNeutrinos
Cline, astro-ph/0103138Cline, astro-ph/0103138
Upper-limit flux ofUpper-limit flux of Kaplinghat et al., Kaplinghat et al., astro-ph/9912391astro-ph/9912391 Integrated 54 cmIntegrated 54 cm-2-2 s s-1-1
Super-K upper limitSuper-K upper limit 29 cm29 cm-2-2 s s-1 -1 for for Kaplinghat et al. Kaplinghat et al. spectrumspectrum [hep-ex/0209028][hep-ex/0209028]
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
DSNB Measurement with Neutron TaggingDSNB Measurement with Neutron Tagging
Beacom & Vagins, hep-ph/0309300 Beacom & Vagins, hep-ph/0309300 [Phys. Rev. Lett., 93:171101, 2004] [Phys. Rev. Lett., 93:171101, 2004]
Pushing the boundaries of neutrinoPushing the boundaries of neutrinoastronomy to cosmological distancesastronomy to cosmological distances
Future large-scale scintillatorFuture large-scale scintillatordetectors (e.g. LENA with 50 kt)detectors (e.g. LENA with 50 kt)
• Inverse beta decay reaction taggedInverse beta decay reaction tagged• Location with smaller reactor fluxLocation with smaller reactor flux (e.g. Pyh(e.g. Pyhääsalmi in Finland) couldsalmi in Finland) could allow for lower thresholdallow for lower threshold
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
LAGUNA - Funded FP7 Design StudyLAGUNA - Funded FP7 Design Study
LLarge arge AApparati for pparati for GGrand rand UUnification and nification and NNeutrino eutrino AAstrophysicsstrophysics(see also arXiv:0705.0116)(see also arXiv:0705.0116)
Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay
The Red Supergiant Betelgeuse (Alpha Orionis)The Red Supergiant Betelgeuse (Alpha Orionis)
First resolvedFirst resolvedimage of a starimage of a starother than Sunother than Sun
DistanceDistance(Hipparcos)(Hipparcos)130 pc (425 lyr)130 pc (425 lyr)
If Betelgeuse goes Supernova:If Betelgeuse goes Supernova:• 66 101077 neutrino events in Super-Kamiokande neutrino events in Super-Kamiokande• 2.42.4 101033 neutron events per day from Silicon-burning phase neutron events per day from Silicon-burning phase (few days warning!), need neutron tagging(few days warning!), need neutron tagging [Odrzywolek, Misiaszek & Kutschera, astro-ph/0311012] [Odrzywolek, Misiaszek & Kutschera, astro-ph/0311012]