Particle-physics lessons from SN 1987A · 1968 1972 1976 1980 1984 1988 1992 1996 2000 2004 MSW...
Transcript of Particle-physics lessons from SN 1987A · 1968 1972 1976 1980 1984 1988 1992 1996 2000 2004 MSW...
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, HawaiiGeorg Raffelt, MaxGeorg Raffelt, Max--PlanckPlanck--Institut für PhysikInstitut für Physik,, MünchenMünchen
Twenty Years After SN 1987A, 23Twenty Years After SN 1987A, 23--25 February 200725 February 2007Hilton Waikola, HawaiiHilton Waikola, Hawaii
ParticleParticle--physics lessons physics lessons from SN 1987Afrom SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Neutrino Burst of Supernova 1987ANeutrino Burst of Supernova 1987A
Within clock uncertainties,Within clock uncertainties,signals are contemporaneoussignals are contemporaneous
KamiokandeKamiokande--II (Japan)II (Japan)Water Cherenkov detectorWater Cherenkov detector2140 tons2140 tonsClock uncertainty Clock uncertainty ±±1 min1 min
IrvineIrvine--MichiganMichigan--Brookhaven (US)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 Clock uncertainty +2/+2/--54 s54 s
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
SN 1987A Signal in LSD (Mont Blanc)SN 1987A Signal in LSD (Mont Blanc) ??
LSD (Liquid Scintillator Detector)LSD (Liquid Scintillator Detector)in the Mont Blanc Tunnelin the Mont Blanc Tunnel(Oct. 1984 (Oct. 1984 -- March 1999)March 1999)Supernova monitor for our galaxySupernova monitor for our galaxy90 tons scintillator90 tons scintillator
200 tons iron (support structure)200 tons iron (support structure)
•• Observed a 5Observed a 5--event clusterevent cluster4.72 hours before IMB/Kam4.72 hours before IMB/Kam--IIII
•• Triggered autmatic SN alertTriggered autmatic SN alert•• Statistical fluctuation very unlikelyStatistical fluctuation very unlikely•• No significant signal in IMB/KamNo significant signal in IMB/Kam--IIII
at LSD timeat LSD time•• No significant LSD signal at IMB timeNo significant LSD signal at IMB time
•• Interpretation as “double bang”:Interpretation as “double bang”:Huge Huge ννee flux (~ 40 MeV) at LSD timeflux (~ 40 MeV) at LSD time
•• LSD signal caused by interactionsLSD signal caused by interactionsin iron of support structurein iron of support structure
•• Second bang ordinary multiSecond bang ordinary multi--flavorflavorsignalsignal
(Imshennik & Ryazhskaya,(Imshennik & Ryazhskaya,“A rotating collapsar and possible“A rotating collapsar and possibleinterpretation of the LSD neutrinointerpretation of the LSD neutrinosignal from SN 1987A”, signal from SN 1987A”, astroastro--ph/0401613) ph/0401613)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
SN 1987A Burst of PapersSN 1987A Burst of Papers
Annual citations in SPIRES of the papers reporting theAnnual citations in SPIRES of the papers reporting theKII, IMB, BST & LSD neutrino observations KII, IMB, BST & LSD neutrino observations (total of 804 citations 1987(total of 804 citations 1987--2006)2006)
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Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Community Interest in NeutrinosCommunity Interest in Neutrinos
Research and conference papers with “neutrino” in title Research and conference papers with “neutrino” in title (SPIRES data base, 22270 “neutrino” papers 1968(SPIRES data base, 22270 “neutrino” papers 1968--2006)2006)
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1968 1972 1976 1980 1984 1988 1992 1996 2000 2004
MSW effectMSW effectSN 1987ASN 1987A
KII & IMBKII & IMBatmosphericatmosphericanomalyanomaly
SuperSuper--K (atmospheric)K (atmospheric)CHOOZCHOOZ
SNO, K2KSNO, K2KKamLandKamLand
LSNDLSNDCHOOZCHOOZ
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
HighestHighest--Impact SN 1987A PapersImpact SN 1987A Papers
Topcite 100+ papers (and a few closely related ones) in SPIRES dTopcite 100+ papers (and a few closely related ones) in SPIRES data base thatata base thatrefer directly to SN 1987A refer directly to SN 1987A νν burst, excluding reviews and papers that mentionburst, excluding reviews and papers that mentionSN 1987A only peripherally (citation count as of 27 January 2007SN 1987A only peripherally (citation count as of 27 January 2007))
Large extraLarge extradimensionsdimensions
Cullen & Perelstein:Cullen & Perelstein:SN 1987A constraints on large compact dimensionsSN 1987A constraints on large compact dimensionsPRL 83:268, 1999 [hepPRL 83:268, 1999 [hep--ph/9903422 ]ph/9903422 ]
270270
AxionsAxions
Raffelt & Seckel:Raffelt & Seckel:Bounds on exotic particle interactions from SN 1987ABounds on exotic particle interactions from SN 1987APRL 60:1793, 1988PRL 60:1793, 1988
209209
Turner:Turner:Axions from SN 1987AAxions from SN 1987APRL 60:1797, 1988PRL 60:1797, 1988
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MayleMayle, , WilsonWilson, , EllisEllis, , OliveOlive, , SchrammSchramm & & SteigmanSteigman::Constraints on axions from SN 1987AConstraints on axions from SN 1987APLB 203:188, 1988PLB 203:188, 1988
9696
EllisEllis & & OliveOlive::Constraints on light particles from supernova SN 1987AConstraints on light particles from supernova SN 1987APLB 203:188, 1988PLB 203:188, 1988
8888
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
HighestHighest--Impact SN 1987A PapersImpact SN 1987A Papers
Topcite 100+ papers (and a few closely related ones) in SPIRES dTopcite 100+ papers (and a few closely related ones) in SPIRES data base thatata base thatrefer directly to SN 1987A refer directly to SN 1987A νν burst, excluding reviews and papers that mentionburst, excluding reviews and papers that mentionSN 1987A only peripherally (citation count as of 27 January 2007SN 1987A only peripherally (citation count as of 27 January 2007))
Large extraLarge extradimensionsdimensions
Cullen & Perelstein:Cullen & Perelstein:SN 1987A constraints on large compact dimensionsSN 1987A constraints on large compact dimensionsPRL 83:268, 1999 [hepPRL 83:268, 1999 [hep--ph/9903422 ]ph/9903422 ]
270270
AxionsAxions
Raffelt & Seckel:Raffelt & Seckel:Bounds on exotic particle interactions from SN 1987ABounds on exotic particle interactions from SN 1987APRL 60:1793, 1988PRL 60:1793, 1988
209209
Turner:Turner:Axions from SN 1987AAxions from SN 1987APRL 60:1797, 1988PRL 60:1797, 1988
144144
MayleMayle, , WilsonWilson, , EllisEllis, , OliveOlive, , SchrammSchramm & & SteigmanSteigman::Constraints on axions from SN 1987AConstraints on axions from SN 1987APLB 203:188, 1988PLB 203:188, 1988
9696
EllisEllis & & OliveOlive::Constraints on light particles from supernova SN 1987AConstraints on light particles from supernova SN 1987APLB 203:188, 1988PLB 203:188, 1988
8888
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Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
David Schramm putting people to work …David Schramm putting people to work …
David SchrammDavid Schramm(Editor Physics Reports)(Editor Physics Reports)
“Why don’t you write a “Why don’t you write a review on astrophysicalreview on astrophysicalaxion limits?”axion limits?”
David SchrammDavid Schramm(Editor Physics Reports)(Editor Physics Reports)
“Why don’t you write a “Why don’t you write a review on astrophysicalreview on astrophysicalaxion limits?”axion limits?”
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
David Schramm putting people to work …David Schramm putting people to work …
David SchrammDavid Schramm(Editor Physics Reports)(Editor Physics Reports)
“Why don’t you write a “Why don’t you write a review on astrophysicalreview on astrophysicalaxion limits?”axion limits?”
David SchrammDavid Schramm(Editor Physics Reports)(Editor Physics Reports)
“Why don’t you write a “Why don’t you write a review on astrophysicalreview on astrophysicalaxion limits?”axion limits?”
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
HighestHighest--Impact SN 1987A PapersImpact SN 1987A Papers
SterileSterileneutrinosneutrinos
Abazajian, Fuller & Patel:Abazajian, Fuller & Patel:Sterile neutrino hot, warm, and cold dark matter Sterile neutrino hot, warm, and cold dark matter PRD 64:023501, 2001 [astroPRD 64:023501, 2001 [astro--ph/0101524] ph/0101524]
9999
NeutrinoNeutrinooscillationsoscillations
Smirnov, Spergel & Bahcall:Smirnov, Spergel & Bahcall:Is large lepton mixing excluded?Is large lepton mixing excluded?PRD 49:1389, 1994 [hepPRD 49:1389, 1994 [hep--ph/9305204] ph/9305204]
115115
Dighe & Smirnov: Identifying the neutrino massDighe & Smirnov: Identifying the neutrino massspectrum from the neutrino burst from a supernovaspectrum from the neutrino burst from a supernovaPRD 62:033007, 2000 [hepPRD 62:033007, 2000 [hep--ph/9907423]ph/9907423]
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Jegerlehner, Neubig & Raffelt:Jegerlehner, Neubig & Raffelt:Neutrino oscillations and the supernova SN 1987A signal Neutrino oscillations and the supernova SN 1987A signal PRD 54:1194, 1996 [astroPRD 54:1194, 1996 [astro--ph/9601111]ph/9601111]
9292
NeutrinoNeutrinodipoledipolemomentsmoments
Barbieri & Mohapatra: Limit on the magnetic momentBarbieri & Mohapatra: Limit on the magnetic momentof the neutrino from supernova SN 1987A observations of the neutrino from supernova SN 1987A observations PRL 61:27, 1988PRL 61:27, 1988
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NNöötzold: New bounds on neutrino magnetic momentstzold: New bounds on neutrino magnetic momentsfrom stellar collapse from stellar collapse PRD 38:1658, 1988PRD 38:1658, 1988
9191
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
HighestHighest--Impact SN 1987A PapersImpact SN 1987A Papers
NucleoNucleo--synthesissynthesis
Woosley, Hartmann, Hoffman & Haxton:Woosley, Hartmann, Hoffman & Haxton:The neutrino processThe neutrino processApJ 356:272, 1990ApJ 356:272, 1990
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SupernovaSupernovaneutrinoneutrinodetectiondetection
Vogel & Beacom:Vogel & Beacom:Angular distribution of neutron inverse beta decayAngular distribution of neutron inverse beta decayPRD 60:053003,1999 [hepPRD 60:053003,1999 [hep--ph/9903554]ph/9903554]
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Burrows, Klein & Gandhi:Burrows, Klein & Gandhi:The future of supernova neutrino detectionThe future of supernova neutrino detectionPRD 45:3361, 1992 PRD 45:3361, 1992
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Haxton: The nuclear response of water CherenkovHaxton: The nuclear response of water Cherenkovdetectors to supernova and solar neutrinos detectors to supernova and solar neutrinos PRD 36:2283, 1987 PRD 36:2283, 1987
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TotaniTotani, , SatoSato, , DalhedDalhed & & WilsonWilson: Future detection of: Future detection ofsupernova neutrino burst and explosion mechanism supernova neutrino burst and explosion mechanism ApJ 496:216,1998 [astroApJ 496:216,1998 [astro--ph/9710203] ph/9710203]
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NeutronNeutron--starstarcoolingcooling
Pons, Reddy, Prakash, Lattimer & Miralles:Pons, Reddy, Prakash, Lattimer & Miralles:Evolution of protoneutron starsEvolution of protoneutron starsApJ 513:780, 1999 [astroApJ 513:780, 1999 [astro--ph/9807040]ph/9807040]
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Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Signal Dispersionand Neutrino Masses
Signal Dispersionand Neutrino Masses
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Some Neutrino Questions in the Late 1980sSome Neutrino Questions in the Late 1980s
FlavorFlavoroscillationsoscillations
•• Solar nu deficit (Homestake)Solar nu deficit (Homestake)•• Not taken very seriously until MSW (~1986)Not taken very seriously until MSW (~1986)
and gallium experiments (~1990)and gallium experiments (~1990)
Now confirmedNow confirmedby manyby manyexperimentsexperiments
MagneticMagneticmomentsmoments
•• Solar flux variation (advocated by R.Davis)Solar flux variation (advocated by R.Davis)Okun, Voloshin & Vysotsky (1986), 580 cit.Okun, Voloshin & Vysotsky (1986), 580 cit.
•• SpinSpin--flavor oscillations flavor oscillations Lim & Marciano (1988), 440 citationsLim & Marciano (1988), 440 citations
•• Akhmedov (1988), 357 citationsAkhmedov (1988), 357 citations
Not dominantNot dominantfor solar nusfor solar nus(KamLAND 2002)(KamLAND 2002)
Are neutrinosAre neutrinosdark matter?dark matter?
•• Dark matter problem widely acknowledgedDark matter problem widely acknowledged•• Nus only candidates among known particlesNus only candidates among known particles•• StructureStructure--formation problemsformation problems•• Nu mass detected in Moscow (17Nu mass detected in Moscow (17−−40 eV)40 eV)
Long sinceLong sinceexcludedexcluded
17 keV17 keVneutrinoneutrino
•• Deformation of Deformation of ββ spectrum in tritium andspectrum in tritium andother isotopes (Simpson 1986 and others)other isotopes (Simpson 1986 and others)
•• About 275 citations, dedicated searchesAbout 275 citations, dedicated searches
InstrumentalInstrumentalerrorerror(A.Hime 1992)(A.Hime 1992)
SecretSecretinteractionsinteractions
Small neutrino masses explained in modelsSmall neutrino masses explained in modelswith a rather strongly coupledwith a rather strongly coupledNambuNambu--Goldstone boson (Majoron)Goldstone boson (Majoron)
Triplet MajoronTriplet Majoronmodel excludedmodel excludedby LEP (~1990)by LEP (~1990)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Neutrino Mass Limits circa 1987Neutrino Mass Limits circa 1987
Review of particle properties 1988Review of particle properties 1988PLB 204 (1988) 1PLB 204 (1988) 195% CL limits95% CL limits
m(m(ννee) < 18 eV) < 18 eVm(m(ννµµ) < 250 keV) < 250 keVm(m(ννττ) < 35 MeV) < 35 MeV
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Hot dark matter ruled out in 1983Hot dark matter ruled out in 1983
1000 particle simulation [Frenk, White & Davis,1000 particle simulation [Frenk, White & Davis, ApJApJ 271 (1983) 417]271 (1983) 417]
The coherence length of the neutrino distribution […] is too larThe coherence length of the neutrino distribution […] is too largegeto be consistent with the observed clustering scale of galaxies to be consistent with the observed clustering scale of galaxies […][…]The conventional neutrinoThe conventional neutrino--dominated picture appears to be ruleddominated picture appears to be ruledout. White,out. White, FrenkFrenk & Davis,& Davis, ApJApJ 274 (1983) L1.274 (1983) L1.
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Nomad and Chorus at CERN (shown at Neutrino 2002)Nomad and Chorus at CERN (shown at Neutrino 2002)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Neutrino Limits by Intrinsic Signal DispersionNeutrino Limits by Intrinsic Signal Dispersion
Time of flight delay by neutrino massTime of flight delay by neutrino mass(G. Zatsepin, JETP Lett. 8:205, 1968)(G. Zatsepin, JETP Lett. 8:205, 1968)
mmννee ≲≲ 20 eV20 eV
•• At the time of SN 1987A At the time of SN 1987A competitive with tritium endcompetitive with tritium end--pointpoint
•• Today mToday mνν << 2.2 eV from tritium2.2 eV from tritium•• Cosmological limit today mCosmological limit today mνν ≲≲ 0.2 eV0.2 eV
22
eV10m
EMeV10
kpc50D
s57.2t ⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛=∆ ν
ν
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kpc50D
s57.2t ⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛=∆ ν
ν
For “milli charged” For “milli charged” neutrinos, neutrinos, pathpath bent by galactic magnetic field, bent by galactic magnetic field, inducing a time delayinducing a time delay
Assuming charge conservation inAssuming charge conservation inneutron decay yields a moreneutron decay yields a morerestrictive limit of about 3restrictive limit of about 3××1010−−2121 ee
122
2B
2103
E6
)dB(ett −
ν
⊥ν ×<=∆ 12
2
2B
2103
E6
)dB(ett −
ν
⊥ν ×<=∆
⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛ µ×<
⊥
−ν
B
17dkpc1
BG1
103e
e⎟⎟⎠
⎞⎜⎜⎝
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⎛ µ×<
⊥
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e
•• Barbiellini & Cocconi,Barbiellini & Cocconi,Nature 329 (1987) 21Nature 329 (1987) 21
•• Bahcall, Neutrino Astrophysics (1989)Bahcall, Neutrino Astrophysics (1989)
Loredo & LambLoredo & LambAnn N.Y. Acad. Sci. 571 (1989) 601Ann N.Y. Acad. Sci. 571 (1989) 601find 23 eV (95% CL limit) from detailedfind 23 eV (95% CL limit) from detailedmaximummaximum--likelihood analysislikelihood analysis
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Some Papers on SN 1987A Neutrino Mass LimitsSome Papers on SN 1987A Neutrino Mass Limits
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Evidence for Cosmologically Interesting Masses?Evidence for Cosmologically Interesting Masses?
If all neutrinos left theIf all neutrinos left theSN at the same time,SN at the same time,evidence for the twoevidence for the twomass values 4 and 22 eVmass values 4 and 22 eV
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Neutrino Mass Sensitivity by Signal DispersionNeutrino Mass Sensitivity by Signal Dispersion
TimeTime--ofof--flight delayflight delayof massive neutrinosof massive neutrinos
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ms1.5t ⎟⎟⎠
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⎛⎟⎟⎠
⎞⎜⎜⎝
⎛=∆ ν
ν
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ms1.5t ⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛=∆ ν
ν
SN 1987ASN 1987A(50 kpc)(50 kpc) mmνν ≲≲ 20 eV20 eV
E E ≈≈ 20 MeV, 20 MeV, ∆∆t t ≈≈ 10 s10 sSimple estimate or detailed maximumSimple estimate or detailed maximumlikelihood analysis give similar resultslikelihood analysis give similar results
Future Future Galactic SNGalactic SNat 10 kpcat 10 kpc(Super(Super--K)K)
mmνν ~ 3 eV~ 3 eVRiseRise--time of signal ~ 10 mstime of signal ~ 10 ms(Totani, PRL 80:2040, 1998)(Totani, PRL 80:2040, 1998)
mmνν ~ 1 eV~ 1 eVFull signalFull signal(Nardi & Zuluaga, NPB 731:140, 2005)(Nardi & Zuluaga, NPB 731:140, 2005)
With lateWith lateblackblack--holeholeformationformation
mmνν ~ 2 eV~ 2 eVCutoff “infinitely” fastCutoff “infinitely” fast(Beacom et al., PRD 63:073011, 2001)(Beacom et al., PRD 63:073011, 2001)
mmνν ~ 1~ 1−−2 eV2 eVD D ≈≈ 750750 kpc, kpc, ∆∆t t ≈≈ 10 s10 sfew tens of eventsfew tens of events
Future SN inFuture SN inAndromedaAndromeda(Megatonne)(Megatonne)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Sensitivity to Time Dependence of SignalSensitivity to Time Dependence of Signal
Maximum neutrinoMaximum neutrino--massmassdispersion for cosmologicaldispersion for cosmologicalmass limit of ~ 0.2 eVmass limit of ~ 0.2 eV
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ms2.0t ⎟⎟⎠
⎞⎜⎜⎝
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⎛=∆ ν
ν
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eV2.0m
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ms2.0t ⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛=∆ ν
ν
Example:Example:Supernova at Supernova at D = 10 kpcD = 10 kpcAccretionAccretion--phase luminosityphase luminosityTimeTime--bins bins bin = 10 msbin = 10 ms
152e serg103)(L −×=ν 152e serg103)(L −×=ν
binms10
%16Signal
nsFluctuatio≈
binms10
%16Signal
nsFluctuatio≈
ms10bin
40bin
Neutrinos≈
ms10bin
40bin
Neutrinos≈
ms10bin
3.6bin
nsFluctuatio≈
ms10bin
3.6bin
nsFluctuatio≈
ms10bin
101.1bin
Photons 4×≈ms10
bin101.1
binPhotons 4×≈
ms10bin
104.2bin
Background 4×≈ms10
bin104.2
binBackground 4×≈
binms10
%6.1Signal
nsFluctuatio≈
binms10
%6.1Signal
nsFluctuatio≈
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
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 300CherenkovCherenkovphotons photons per OMper OMfrom a SNfrom a SNat 10 kpcat 10 kpc
•• NoiseNoiseper OMper OM< 500 Hz< 500 Hz
•• Total ofTotal of4800 OMs4800 OMsin 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[Dighe, Keil & Raffelt, hep--ph/0303210]ph/0303210]
Method first discussed byMethod first discussed by•• Pryor, Roos & Webster,Pryor, Roos & Webster,
ApJ 329:355 (1988)ApJ 329:355 (1988)•• HalzenHalzen, , JacobsenJacobsen & & ZasZas
astroastro--ph/9512080ph/9512080
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Dispersion between Neutrinos and PhotonsDispersion between Neutrinos and Photons
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 withinSN 1987A: Transit time for photons and neutrinos equal to within ~ 3h~ 3h
Equal within ~ 1 Equal within ~ 1 −− 4 4 ××1010−−33
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 Proves directly that neutrinos respond to gravity in the usual waywaybecause for photons gravitational lensing already proves thisbecause for photons gravitational lensing already proves this pointpoint
•• Cosmological limits Cosmological limits ∆∆NNνν ≲≲ 1 much worse test of neutrino gravitation,1 much worse test of neutrino gravitation,i.e. SN 1987A proves that neutrinos in cosmology gravitate asi.e. SN 1987A proves that neutrinos in cosmology gravitate as they shouldthey should
•• Provides limits on parameters of certain nonProvides limits on parameters of certain non--GR theories of gravitationGR theories of gravitation•• Photons likely obscured for next galactic SN, so this result prPhotons likely obscured for next galactic SN, so this result probablyobably
unique to SN 1987A unique to SN 1987A
∫ months51dt)]t(r[U2t BAShapiro −≈−=∆ ∫ months51dt)]t(r[U2t BAShapiro −≈−=∆
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
GammaGamma--Ray Observations of SMM SatelliteRay Observations of SMM Satellite
Counts in the GRS instrument on the Solar Maximum Mission SatellCounts in the GRS instrument on the Solar Maximum Mission Satelliteite
SN 1987ASN 1987A 10s fluence10s fluencelimitslimits
0.4 cm0.4 cm−−22
0.6 cm0.6 cm−−22
SN 1987A neutrino fluence ~ 10SN 1987A neutrino fluence ~ 101010 cmcm−−22 << 1010−−1010 of neutrinos haveof neutrinos havedecayed between SN and Earthdecayed between SN and Earth
0.9 cm0.9 cm−−22
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Neutrino Radiative Lifetime LimitsNeutrino Radiative Lifetime Limits
PlasmondecayPlasmondecay
RadiativedecayRadiativedecay
′ν → ν + γ′ν → ν + γ
For lowFor low--massmassneutrinos,neutrinos,plasmon decayplasmon decayin globularin globularcluster starscluster starsyields mostyields mostrestrictive limitsrestrictive limits
32eff m8 νγν′→ν π
µ=Γ 3
2eff m8 νγν′→ν π
µ=Γ
3pl
2eff
24ω
π
µ=Γ νν→γ
3pl
2eff
24ω
π
µ=Γ νν→γ
ν+ν→γpl ν+ν→γpl
RaffeltRaffelt, PRL 81:4020,1998 [astro, PRL 81:4020,1998 [astro--ph/9808299] ph/9808299]
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Energy-loss limits onneutrinos and axionsEnergy-loss limits onneutrinos and axions
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
LateLate--time signal most sensitive observabletime signal most sensitive observable
The EnergyThe Energy--Loss ArgumentLoss Argument
NeutrinoNeutrinospheresphere
NeutrinoNeutrinodiffusiondiffusion
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 emissionof novel particlesof novel particles
SN 1987A neutrino signalSN 1987A neutrino signal
εεxx << 10101919 erg gerg g−−11 ss−−11
Assuming that the neutrino burst was notAssuming that the neutrino burst was notshortened by more than ~ ½ leads to anshortened by more than ~ ½ leads to anapproximate requirement on a novelapproximate requirement on a novelenergyenergy--loss rate ofloss rate of
for for ρρ ≈≈ 3 3 ×× 10101414 g cmg cm−−33 and T and T ≈≈ 30 MeV30 MeV
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Dirac NeutrinosDirac Neutrinos
•• If neutrinos are Dirac particles, rightIf neutrinos are Dirac particles, right--handed states existhanded states existthat do not interact by ordinary weak interactionsthat do not interact by ordinary weak interactions
•• Couplings are constrained by SN 1987A energyCouplings are constrained by SN 1987A energy--loss argumentloss argument
eRνeRνee
ppRWRWRightRight--handedhanded
currentscurrentsnn
GGRR ≲≲ 1010−−55 GGFF
0Z0ZLνLν RνRν
Dirac massDirac massNN NN
mmDD ≲≲ 30 keV30 keV
γγLνLν RνRν
pp
DipoleDipolemomentsmoments pp
µµνν ≲≲ 1010−−1212 µµBB
RνRν
RνRν
γγMilli chargeMilli charge eeνν ≲≲ 1010−−99 ee
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
RightRight--Handed Neutrinos in the Early UniverseHanded Neutrinos in the Early Universe
•• If neutrinos are Dirac particles, will the rightIf neutrinos are Dirac particles, will the right--handed componentshanded componentsachieve thermal equilibrium in the early universe before bigachieve thermal equilibrium in the early universe before big--bangbangnucleosythesis?nucleosythesis?
•• This would modify the lightThis would modify the light--element abundances in significant ways,element abundances in significant ways,notably increase the helium abundancenotably increase the helium abundance
Required strengthRequired strength SN 1987A limitSN 1987A limit
RightRight--handedhandedcharged currentcharged current GGRR ~ 10~ 10−−33 GGFF GGRR ≲≲ 1010−−55 GGFF
Dirac massDirac mass few 100 keVfew 100 keV 30 keV30 keV
Dipole momentDipole moment ~ 0.5 x 10~ 0.5 x 10−−1010 µµBB 1010−−1212 µµBB
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Sterile NeutrinosSterile Neutrinos
To avoid complete energy loss in ~ 1 sTo avoid complete energy loss in ~ 1 s
sinsin22(2(2ΘΘeses) ) ≲≲ 3 3 ×× 1010−−1010
Average scattering rate in SN coreAverage scattering rate in SN coreinvolving ordinary leftinvolving ordinary left--handed neutrinoshanded neutrinos
110L s10 −≈Γ 110L s10 −≈Γ
Electron neutrino appears as sterile neutrinoElectron neutrino appears as sterile neutrinoin ½ sinin ½ sin22(2(2ΘΘeses) of all cases) of all cases
Les2
21
s )2(sin ΓΘ≈Γ Les2
21
s )2(sin ΓΘ≈Γ
1110es
221 s1s10)2(sin −− <Θ 1110
es2
21 s1s10)2(sin −− <Θ
ActiveActive--sterilesterilemixingmixing
sνsνee
ppWW
nn
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Sterile Neutrino LimitsSterile Neutrino Limits
See also:See also:
MaalampiMaalampi & & PeltoniemiPeltoniemi::Effects of the 17Effects of the 17--keVkeVneutrino in supernovae neutrino in supernovae PLB 269:357,1991PLB 269:357,1991
HidakaHidaka & & FullerFuller::Dark matter sterileDark matter sterileneutrinos in stellarneutrinos in stellarcollapse: alteration ofcollapse: alteration ofenergy/lepton numberenergy/lepton numbertransport and atransport and amechanism formechanism forsupernova explosionsupernova explosionenhancementenhancementPRD 74:125015,2006 PRD 74:125015,2006
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Axion Emission from a Nuclear MediumAxion Emission from a Nuclear Medium
AxionAxion--nucleon interactionnucleon interactionis of currentis of current--current form:current form:
aJf2
Ca
f2C
L A
a
NN5N
a
Nint
µµ
µµ ∂=∂ΨγγΨ= aJ
f2C
af2
CL A
a
NN5N
a
Nint
µµ
µµ ∂=∂ΨγγΨ=
Difficulties include:Difficulties include:•• Realistic nucleonRealistic nucleon--nucleon interaction potential (even in vacuum) nucleon interaction potential (even in vacuum) •• ManyMany--body effects (effective mass, spinbody effects (effective mass, spin--spin correlations ...)spin correlations ...)•• Axion couplings in the nuclear mediumAxion couplings in the nuclear medium•• MultipleMultiple--scattering effects: scattering effects: Frequency of NN collisions exceeds typical axion energyFrequency of NN collisions exceeds typical axion energyττcollcoll << ωω−−11
Expect LPMExpect LPM--type destructive interference effectstype destructive interference effects
NN
NN
NN
NNVV
NucleonNucleon--NucleonNucleonBremsstrahlungBremsstrahlung
+ ...+ ...
aa Energy loss rate (erg cmEnergy loss rate (erg cm−−33 ss−−11)) AxionAxionenergyenergy
DynamicalDynamicalstructurestructurefunctionfunction∫
∫∫∞
ω−ωωπ⎟⎟
⎠
⎞⎜⎜⎝
⎛=
ωΓΓ=
0
42
B2
a
N
2Nucleonsa
)(Sd4
nf2
C
MddQ
∫
∫∫∞
ω−ωωπ⎟⎟
⎠
⎞⎜⎜⎝
⎛=
ωΓΓ=
0
42
B2
a
N
2Nucleonsa
)(Sd4
nf2
C
MddQ
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Axion Emission from a Nuclear MediumAxion Emission from a Nuclear Medium
AxionAxion--nucleon interactionnucleon interactionis of currentis of current--current form:current form:
aJf2
Ca
f2C
L A
a
NN5N
a
Nint
µµ
µµ ∂=∂ΨγγΨ= aJ
f2C
af2
CL A
a
NN5N
a
Nint
µµ
µµ ∂=∂ΨγγΨ=
Difficulties include:Difficulties include:•• Realistic nucleonRealistic nucleon--nucleon interaction potential (even in vacuum) nucleon interaction potential (even in vacuum) •• ManyMany--body effects (effective mass, spinbody effects (effective mass, spin--spin correlations ...)spin correlations ...)•• Axion couplings in the nuclear mediumAxion couplings in the nuclear medium•• MultipleMultiple--scattering effects: scattering effects: Frequency of NN collisions exceeds typical axion energyFrequency of NN collisions exceeds typical axion energyττcollcoll << ωω−−11
Expect LPMExpect LPM--type destructive interference effectstype destructive interference effects
NN
NN
NN
NNVV
NucleonNucleon--NucleonNucleonBremsstrahlungBremsstrahlung
+ ...+ ...
aa Energy loss rate (erg cmEnergy loss rate (erg cm−−33 ss−−11)) AxionAxionenergyenergy
DynamicalDynamicalstructurestructurefunctionfunction∫
∫∫∞
ω−ωωπ⎟⎟
⎠
⎞⎜⎜⎝
⎛=
ωΓΓ=
0
42
B2
a
N
2Nucleonsa
)(Sd4
nf2
C
MddQ
∫
∫∫∞
ω−ωωπ⎟⎟
⎠
⎞⎜⎜⎝
⎛=
ωΓΓ=
0
42
B2
a
N
2Nucleonsa
)(Sd4
nf2
C
MddQ
•• Fundamentally the dynamical structure function isFundamentally the dynamical structure function isa correlator of the nucleon axial currenta correlator of the nucleon axial current
•• NonNon--relativistic nucleons: ~ nucleon spin density operator relativistic nucleons: ~ nucleon spin density operator σσ
•• Example for the fluctuation and dissipation theoremExample for the fluctuation and dissipation theoremof linearof linear--response theory: Axion emission determined byresponse theory: Axion emission determined byspontaneous nucleon spin fluctuationsspontaneous nucleon spin fluctuations
)k,0()k,t(edtn34
)k,(S ti
B−σ⋅σ=ω ω
∞+
∞−∫
rr )k,0()k,t(edtn34
)k,(S ti
B−σ⋅σ=ω ω
∞+
∞−∫
rr
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Properties of the Dynamical Structure FunctionProperties of the Dynamical Structure Function
Nucleon spinNucleon spin--density density autocorrelation functionautocorrelation function
Normalization, ignoringNormalization, ignoringmanymany--body correlationsbody correlations
LongLong--wavelength limitwavelength limit(k (k →→ 0)0)
Is Fourier transform ofIs Fourier transform ofsinglesingle--nucleonnucleonspin correlation functionspin correlation function
Symmetric formSymmetric form
Detailed balancingDetailed balancingconsequence ofconsequence ofnonnon--commuting commuting σσ(t) (t) at different times at different times
∫∞+
∞−
ω −σ⋅σ=ω )k,0()k,t(edtn34
)k,(S ti
B
rr∫∞+
∞−
ω −σ⋅σ=ω )k,0()k,t(edtn34
)k,(S ti
B
rr
∫∫ +∞+
∞−−
π=ω
πω
)f1(f)2(
pd2n1
)k,(S2d
kpp3
3
B∫∫ +
∞+
∞−−
π=ω
πω
)f1(f)2(
pd2n1
)k,(S2d
kpp3
3
B
)k,(Se)k,(S T/ ω=ω− ω− )k,(Se)k,(S T/ ω=ω− ω−
2)k,(S)k,(S
)k,(Sω+ω−
=ω2
)k,(S)k,(S)k,(S
ω+ω−=ω T/e1
)k,(S2)k,(S ω−+
ω=ω T/e1
)k,(S2)k,(S ω−+
ω=ω
2)t(s)0(s)0(s)t(s
edt34
)(S tirrrr
⋅+⋅=ω ∫
∞+
∞−
ω2
)t(s)0(s)0(s)t(sedt
34
)(S tirrrr
⋅+⋅=ω ∫
∞+
∞−
ω
2)t(s)0(s)0(s)t(s
34
)t(Rrrrr
⋅+⋅=
2)t(s)0(s)0(s)t(s
34
)t(Rrrrr
⋅+⋅=
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Spin Relaxation RateSpin Relaxation Rate
Identify coefficient Identify coefficient Γ Γ fromfrombremsstrahlung calculationbremsstrahlung calculationwith spin relaxation ratewith spin relaxation rate
Generic form for singleGeneric form for singlecollisions & small energiescollisions & small energies
22)(S ωΓ=ω 22)(S ωΓ=ω
NN
NN
NN
NNVV
NucleonNucleon--NucleonNucleonBremsstrahlungBremsstrahlung
+ ...+ ...
aa
A spin immersed in a bath of scatterers with spinA spin immersed in a bath of scatterers with spin--dependent forces dependent forces relaxes exponentially for uncorrelated kicks (Markov chain)relaxes exponentially for uncorrelated kicks (Markov chain)
with with ΓΓ the “spin relaxation rate”, leading to the Fourier transformthe “spin relaxation rate”, leading to the Fourier transformLorentzian structure function,Lorentzian structure function,includes multiple scattering effectsincludes multiple scattering effects
te)t(R Γ−= te)t(R Γ−=
222
)(SΓ+ω
Γ=ω 22
2)(S
Γ+ω
Γ=ω
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Standard behavior:Standard behavior:Bremsstrahlung rate Bremsstrahlung rate ∝∝ ρρ22
Including LPM effectIncluding LPM effect
Axion Emission RateAxion Emission Rate
for small densityfor small density
for large densityfor large density
Axionic volume energy loss rate ofAxionic volume energy loss rate ofnuclear mediumnuclear medium
⎪⎩
⎪⎨⎧
∝+Γ+ω
Γωω
π⎟⎟⎠
⎞⎜⎜⎝
⎛=
ω−ωωπ⎟⎟
⎠
⎞⎜⎜⎝
⎛=
−ω
∞
∞
∫
∫
1B
2B
T/0
224
2B
2
a
N
0
42
B2
a
N
n
n
e1
22d
4
nf2
C
)(Sd4
nf2
CQ
⎪⎩
⎪⎨⎧
∝+Γ+ω
Γωω
π⎟⎟⎠
⎞⎜⎜⎝
⎛=
ω−ωωπ⎟⎟
⎠
⎞⎜⎜⎝
⎛=
−ω
∞
∞
∫
∫
1B
2B
T/0
224
2B
2
a
N
0
42
B2
a
N
n
n
e1
22d
4
nf2
C
)(Sd4
nf2
CQ
OneOne--pion exchange potential in pion exchange potential in Born approximation:Born approximation:
TMeV30
cmg1025.1
T 314 −ρ
≈Γ
TMeV30
cmg1025.1
T 314 −ρ
≈Γ
Using phase shifts fromUsing phase shifts fromnuclear scattering data nuclear scattering data (Hanhart, Phillips & Reddy,(Hanhart, Phillips & Reddy,astroastro--ph/0003445)ph/0003445)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
SN 1987A Axion LimitsSN 1987A Axion Limits
ExcludedExcluded
SN coreSN coreSN coreSN core
NeutrinoNeutrinodiffusiondiffusion
NeutrinoNeutrinodiffusiondiffusion
TrappingTrapping
Burrows, RessellBurrows, Ressell& Turner,& Turner,PRD 42:3297,1990PRD 42:3297,1990
AxionAxiondiffusiondiffusion
Free streamingFree streaming
Burrows, TurnerBurrows, Turner& Brinkmann,& Brinkmann,PRD 39:1020,1989PRD 39:1020,1989
Volume emissionVolume emissionof axionsof axions
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
DirectDirectsearchsearch
Cold Dark MatterCold Dark Matter
TeleTelescopescopeExperimentsExperiments
Globular clustersGlobular clusters(a(a--γγ--coupling)coupling)
Too manyToo manyeventsevents
Too muchToo muchenergy lossenergy loss
SN 1987A (aSN 1987A (a--NN--coupling)coupling)
Astrophysical Axion BoundsAstrophysical Axion Bounds
101033 101066 101099 10101212 [[GeVGeV]] ffaa
eVeVkeVkeV meVmeV µµeVeVmmaa
Hot dark matter limitsHot dark matter limits(a(a--ππ--coupling)coupling)
CASTCAST ADMXADMX
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Improving EnergyImproving Energy--Loss Limits with Next Supernova?Loss Limits with Next Supernova?
•• Even a relatively lowEven a relatively low--statistics new measurment could confirmstatistics new measurment could confirmgeneral validity of SN 1987A energygeneral validity of SN 1987A energy--loss limitsloss limits(i.e. make sure that we were not fooled by sparse data)(i.e. make sure that we were not fooled by sparse data)
•• A galactic SN even in a small detector orA galactic SN even in a small detector ora SN in Andromeda with a megatonne detectora SN in Andromeda with a megatonne detectorwould be extremely usefulwould be extremely useful
•• Granted this, the main uncertainties are theoreticalGranted this, the main uncertainties are theoretical(conditions and processes in hot and dense nuclear medium)(conditions and processes in hot and dense nuclear medium)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Signatures forNeutrino Oscillations?
Signatures forNeutrino Oscillations?
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
LevelLevel--Crossing Diagram in a SN EnvelopeCrossing Diagram in a SN Envelope
Dighe & Smirnov, Identifying the neutrino mass spectrum from a sDighe & Smirnov, Identifying the neutrino mass spectrum from a supernovaupernovaneutrino burst, astroneutrino burst, astro--ph/9907423ph/9907423
Normal mass hierarchyNormal mass hierarchy Inverted mass hierarchyInverted mass hierarchy
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Spectra Emerging from SupernovaeSpectra Emerging from Supernovae
Primary fluxesPrimary fluxes
for for
for for
for for
0eF0eF0eF0eF0xF0xF
eνeν
eνeν
ττµµ νννν ,,, ττµµ νννν ,,,
After leaving theAfter leaving thesupernova envelope,supernova envelope,the fluxes arethe fluxes arepartially swappedpartially swapped
0x
0e
0e F)p1(FpF −+= 0
x0e
0e F)p1(FpF −+=
0x
0e
0e F)p1(FpF −+= 0
x0e
0e F)p1(FpF −+=
0e
0e
0xx4
1 F4
p1F
4p1
F4
pp2F
−+
−+
++=∑ 0
e0e
0xx4
1 F4
p1F
4p1
F4
pp2F
−+
−+
++=∑
NormalNormal
InvertedInverted
sinsin22(2(2ΘΘ1313))
≲≲ 1010−−55
≳≳ 1010−−33
AnyAny
Mass orderingMass ordering
sinsin22((ΘΘ1212)) ≈≈ 0.30.3
00 coscos22((ΘΘ1212)) ≈≈ 0.70.7
sinsin22((ΘΘ1212)) ≈≈ 0.30.3 coscos22((ΘΘ1212)) ≈≈ 0.70.7
00
CaseCase
AA
BB
CC
Survival probabilitySurvival probability
)for(p eν )for(p eν )for(p eν )for(p eν
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Interpreting SN 1987A NeutrinosInterpreting SN 1987A Neutrinos
Tota
l Bin
ding
Ene
rgy
Tota
l Bin
ding
Ene
rgy
95 % CLContours
Jegerlehner, Jegerlehner, Neubig & Raffelt,Neubig & Raffelt,PRD 54 (1996) 1194PRD 54 (1996) 1194
Assume thermalAssume thermalspectra andspectra andequipartition ofequipartition ofenergy between energy between the six degrees the six degrees of freedom of freedom ννee,, ννµµ,, ννττ and theirand theirantiparticlesantiparticlesSpectral Spectral ννee TemperatureTemperature
__
TheoryTheory
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
SN 1987A, Earth matter effect and LMASN 1987A, Earth matter effect and LMA
From C. Lunardini’s From C. Lunardini’s Talk in LA (Feb 01) Talk in LA (Feb 01)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
SN 1987A and Earth Matter EffectSN 1987A and Earth Matter Effect
KamiokandeKamiokande
IMBIMB
Lunardini & SmirnovLunardini & Smirnovhephep--ph/0009356ph/0009356
Oscillation onlyOscillation onlyin supernovain supernova
Include EarthInclude Eartheffecteffect
5.0)2cos( =θ 5.0)2cos( =θ252 eV1075.2m −×=∆ 252 eV1075.2m −×=∆
MeV5.3)(T e =ν MeV5.3)(T e =ν
MeV0.7)(T =νµ MeV0.7)(T =νµ
Only events up 6.5 sOnly events up 6.5 s
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
SN 1987A and Earth Matter EffectSN 1987A and Earth Matter Effect
Lunardini & SmirnovLunardini & Smirnovhephep--ph/0009356ph/0009356
TheoryTheory
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
FlavorFlavor--Dependent Fluxes and SpectraDependent Fluxes and Spectra
Broad characteristicsBroad characteristics•• Duration a few secondsDuration a few seconds•• ⟨⟨EEνν⟩⟩ ~ ~ 1010−−20 MeV20 MeV•• ⟨⟨EEνν⟩⟩ increases with timeincreases with time•• Hierarchy of energiesHierarchy of energies
•• Approximate equipartitionApproximate equipartitionof energy between flavorsof energy between flavors
xee EEE ννν << xee EEE ννν <<
Livermore numerical modelLivermore numerical modelApJ 496 (1998) 216ApJ 496 (1998) 216
Prompt Prompt ννeedeleptonizationdeleptonizationburstburst
ννee
ννee
ννxx__
However, in traditionalHowever, in traditionalsimulations transport simulations transport of of ννµµ and and ννττ schematicschematic
•• Incomplete microphysicsIncomplete microphysics
•• Crude numerics to coupleCrude numerics to coupleneutrino transport withneutrino transport withhydro codehydro code
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Supernova Neutrino Spectra FormationSupernova Neutrino Spectra Formation
Electron flavorElectron flavor (( ))ee,νν ee,νν
Free Free streamingstreaming−↔ν epne
−↔ν epne
+↔ν enpe+↔ν enpe
Thermal Equilibrium
Neutrino sphere (TNeutrino sphere (TNSNS))
Other flavorsOther flavors (( ))τµτµ νννν ,,, τµτµ νννν ,,,
DiffusionDiffusionThermal Equilibrium
Scattering AtmosphereScattering Atmosphere
ν↔ν NN ν↔ν NN
ν↔ν NN ν↔ν NN
νν↔ NNNN νν↔ NNNNνν↔−+ee νν↔−+ee
ee ν↔ν ee ν↔ν
Free Free streamingstreaming
µνµν↔νν ee µνµν↔νν ee
Transport sphereTransport sphereEnergy sphere (TEnergy sphere (TESES))
Raffelt (astroRaffelt (astro--ph/0105250), Keil, Raffelt & Janka (astroph/0105250), Keil, Raffelt & Janka (astro--ph/0208035)ph/0208035)
TTfluxflux~~ TTNSNS
TTfluxflux~0.6T~0.6TESES
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
Literature Scan of FlavorLiterature Scan of Flavor--Dependent Neutrino SpectraDependent Neutrino Spectra
Keil, Janka & Raffelt, astroKeil, Janka & Raffelt, astro--ph/0208035ph/0208035
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
FlavorFlavor--Dependent Neutrino Fluxes vs. Equation of StateDependent Neutrino Fluxes vs. Equation of State
Kitaura, Janka & Hillebrandt, “Explosions of OKitaura, Janka & Hillebrandt, “Explosions of O--NeNe--Mg cores, the CrabMg cores, the Crabsupernova, and subluminous Type IIsupernova, and subluminous Type II--P supernovae”, astroP supernovae”, astro--ph/0512065ph/0512065
Wolff & Hillebrandt nuclear EoS (stiff)
eνeν
τµτµ νν ,, ,
Lattimer & Swesty nuclear EoS (soft)
eνeν
τµτµ νν ,, ,
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
So what have we learnt? What can we learn?So what have we learnt? What can we learn?
No unexpected energyNo unexpected energy--loss channel:loss channel:Restrictive limits on axions, large extraRestrictive limits on axions, large extradimensions, rightdimensions, right--handed neutrinoshanded neutrinos(couplings, mixings, dipole moments),(couplings, mixings, dipole moments),Majorons, light SUSY particles, …Majorons, light SUSY particles, …
Should be generally confirmedShould be generally confirmed(low(low--statistics signal enough),statistics signal enough),but uncertainty dominated by theorybut uncertainty dominated by theory(processes in a dense nuclear medium)(processes in a dense nuclear medium)
Neutrinos gravitate as expectedNeutrinos gravitate as expected(Shapiro(Shapiro timetime delaydelay relativerelative toto photons)photons)
Requires photon observations (IR ifRequires photon observations (IR ifobscured) and depends on distanceobscured) and depends on distance
Nothing useful about absolute mNothing useful about absolute mνν Time variation of signal in IceCube?Time variation of signal in IceCube?
•• Nothing useful about oscillationsNothing useful about oscillations•• Hints that flavor dependence ofHints that flavor dependence of
spectra indeed is not largespectra indeed is not large
Neutrino mass hierarchy and/orNeutrino mass hierarchy and/orinformation on information on ΘΘ13 13 (with luck)(with luck)
General confirmation of coreGeneral confirmation of core--collapsecollapseparadigm paradigm (total energy, spectra, time scale)(total energy, spectra, time scale)
•• Detailed test by highDetailed test by high--statistics signalstatistics signal•• Detection of unexpected featuresDetection of unexpected features
SN 1987ASN 1987A Future supernovaFuture supernova
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Twenty Years After SN 1987A, 23-25 February 2007, Hilton Waikola, Hawaii
SN 1006SN 1006
Looking forward to the lessons from theLooking forward to the lessons from thenext galactic supernovanext galactic supernova
http://antwrp.gsfc.nasa.gov/apod/ap060430.htmlhttp://antwrp.gsfc.nasa.gov/apod/ap060430.html