Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH AachenTitle Georg Raffelt, Max-Planck-Institut für Physik,
Post on 05-Apr-2015
106 Views
Preview:
Transcript
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
TitleTitle
Georg Raffelt, Max-Planck-Institut für Physik, Georg Raffelt, Max-Planck-Institut für Physik, MünchenMünchen
Physik Kolloquium,Physik Kolloquium, 19.19. November 2007November 2007
RWTH AachenRWTH AachenExzellenzExzellenz
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Aachen SkylineAachen Skyline
Supernova Neutrinos20 Years after SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Crab NebulaCrab Nebula
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Supernova 1054 PetrographSupernova 1054 Petrograph
Possible SN 1054 Petrograph by the Anasazi peoplePossible SN 1054 Petrograph by the Anasazi people(Chaco Canyon, New Mexico)(Chaco Canyon, New Mexico)
CrescentCrescentMoonMoon
3 concentric circles, 3 concentric circles, diameter diameter 1 foot, 1 foot, with huge red flameswith huge red flamestrailing to the right.trailing to the right.(Halley’s Comet(Halley’s Comet ?)?)
SN 1054SN 1054
Hand signifiesHand signifiessacred placesacred place
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Periodic System of Elementary ParticlesPeriodic System of Elementary Particles
QuarksQuarks LeptonsLeptons
Charge Charge 2/3 2/3
Up Up
Charge Charge 1/3 1/3
Down Down
Charge Charge 1 1
Electron Electron
Charge Charge 00
e-Neutrino e-Neutrino eeeedduu
NeutronNeutron
ProtonProton
QuarksQuarks LeptonsLeptons
Charm Charm
Top Top
Gravitation Gravitation
Weak InteractionWeak Interaction
Strong Interaction (QCD)Strong Interaction (QCD)
Electromagnetic Interaction (QED)Electromagnetic Interaction (QED)
Down Down
Strange Strange
Bottom Bottom
Electron Electron
Muon Muon
Tau Tau
e-Neutrino e-Neutrino
-Neutrino -Neutrino
1st Family1st Family
2nd Family 2nd Family
3rd Family3rd Family
Charge Charge 2/3 2/3 Charge Charge 1/3 1/3 Charge Charge 1 1 Charge Charge 00
Up Up
-Neutrino -Neutrino
eeee
dd
ss
bb
cc
tt
uu
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Super-Kamiokande Neutrino DetectorSuper-Kamiokande Neutrino Detector
42 m42 m
39.3 39.3 mm
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Cherenkov RingCherenkov Ring
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Super-Kamiokande: Sun in the Light of Super-Kamiokande: Sun in the Light of NeutrinosNeutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
SN 1987A Event No.9 in Kamiokande-II SN 1987A Event No.9 in Kamiokande-II
Kamiokande-II detectorKamiokande-II detector2140 tons of water fiducial volume2140 tons of water fiducial volumefor SN 1987Afor SN 1987A
Hirata et al., PRD 38 (1988) 448Hirata et al., PRD 38 (1988) 448
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Some Particle-Physics Some Particle-Physics Lessons from SN 1987ALessons from SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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)
mmee ≲≲ 20 eV20 eV
• At the time of SN 1987A At the time of SN 1987A competitive with tritium end-pointcompetitive with tritium end-point
• Today mToday m << 2.2 eV from tritium 2.2 eV from tritium
• Cosmological limit today mCosmological limit today m ≲≲ 0.2 eV 0.2 eV
22
eV10m
EMeV10
kpc50D
s57.2t
22
eV10m
EMeV10
kpc50D
s57.2t
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 310102121 e e
122
2B
2103
E6
)dB(ett
12
2
2B
2103
E6
)dB(ett
B
17dkpc1
BG1
103e
e
B
17dkpc1
BG1
103e
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 detailedmaximum-likelihood analysismaximum-likelihood analysis
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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• Photons likely obscured for next galactic SN, so this result probablyPhotons likely obscured for next galactic SN, so this result probably 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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Core-CollapseCore-CollapseExplosion MechanismExplosion Mechanism
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Delayed ExplosionDelayed Explosion
Wilson, Proc. Univ. Illinois Meeting on Num. Astrophys.(1982)Wilson, Proc. Univ. Illinois Meeting on Num. Astrophys.(1982)Bethe & Wilson, ApJ 295 (1985) 14Bethe & Wilson, ApJ 295 (1985) 14
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Galactic Supernova RateGalactic Supernova Rate
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Local Group of GalaxiesLocal Group of Galaxies
250250
6060
3030
Events in a detector withEvents in a detector with 30 x Super-K fiducial volume,30 x Super-K fiducial volume, e.g. Hyper-Kamiokandee.g. Hyper-Kamiokande
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Nearby Galaxies with Many Observed Nearby Galaxies with Many Observed SupernovaeSupernovae
M83 (NGC 5236, Southern Pinwheel)M83 (NGC 5236, Southern Pinwheel)D = 4.5 MpcD = 4.5 Mpc
Observed Supernovae: Observed Supernovae: 1923A, 1945B, 1950B,1923A, 1945B, 1950B, 1957D, 1968L, 1983N 1957D, 1968L, 1983N
NGC 6946 NGC 6946 D = (5.5 ± 1) MpcD = (5.5 ± 1) Mpc
Observed Supernovae:Observed Supernovae: 1917A, 1939C, 1948B, 1968D,1917A, 1939C, 1948B, 1968D, 1969P, 1980K, 2002hh, 2004et1969P, 1980K, 2002hh, 2004et
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Future SupernovaFuture SupernovaNeutrino ObservationsNeutrino Observations
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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• 22 of 80 strings installed (2007)22 of 80 strings installed (2007)• Completion until 2011 foreseenCompletion until 2011 foreseen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
SupernovaSupernovaNeutrino OscillationsNeutrino Oscillations
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Mixing of Neutrinos with Different MassMixing of Neutrinos with Different Mass
ElectronElectronneutrinoneutrino
NeutrinoNeutrinomass mmass m11
NeutrinoNeutrinomass mmass m22
Neutrino propagation as a wave phenomenonNeutrino propagation as a wave phenomenon
Mass mMass m11
Mass mMass m2 2 = m= m11
Mass mMass m11
Mass mMass m2 2 >> m m11
Mass mMass m11
Mass mMass m2 2 >> m m11
Mass mMass m11
Mass mMass m2 2 >> m m11
Mass mMass m11
Mass mMass m22 >> m m11
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Neutrino OscillationsNeutrino Oscillations
Mass mMass m11
Mass mMass m22 >> m m11Oscillation lengthOscillation length
21
22 mm
E4
21
22 mm
E4
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Neutrino OscillationsNeutrino Oscillations
Oscillation lengthOscillation length
21
22 mm
E4
21
22 mm
E4
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Long-Baseline Experiment K2KLong-Baseline Experiment K2K
K2K ExperimentK2K Experiment(KEK to (KEK to Kamiokande)Kamiokande)has confirmedhas confirmedneutrinoneutrinooscillations,oscillations,to be followedto be followedby T2K (2009)by T2K (2009)
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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
In Earth or Sun weak In Earth or Sun weak potentialpotential
of order 10of order 101313 eV eV
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Matrices of Density in Flavor SpaceMatrices of Density in Flavor Space
Neutrino quantum fieldNeutrino quantum field
Spinors in flavor spaceSpinors in flavor space
Quantum states (amplitudes)Quantum states (amplitudes)
Variables for discussing neutrino flavor oscillationsVariables for discussing neutrino flavor oscillations
““Matrices of densities” Matrices of densities” (analogous to occupation numbers)(analogous to occupation numbers)
““Quadratic” quantities, required forQuadratic” quantities, required fordealing with decoherence, collisions,dealing with decoherence, collisions,Pauli-blocking, nu-nu-refraction, etc.Pauli-blocking, nu-nu-refraction, etc.
Sufficient for “beam experiments,”Sufficient for “beam experiments,”but confusing “wave packet debates”but confusing “wave packet debates”for quantifying decoherence effectsfor quantifying decoherence effects
xpi
p†
p3
3evp,tbup,ta
2
pd)x,t(
xpi
p†
p3
3evp,tbup,ta
2
pd)x,t(
3
2
1
3
2
1
3
2
1
a
a
a
a
3
2
1
a
a
a
a
3
2
1
b
b
b
b
3
2
1
b
b
b
bDestructionDestructionoperators foroperators for(anti)neutrinos(anti)neutrinos
0
a
p,ta
p,ta
p,t
p,t
p,t†
p,t3
2
1
3
2
1
0
a
p,ta
p,ta
p,t
p,t
p,t†
p,t3
2
1
3
2
1
NeutrinosNeutrinos
Anti-Anti-neutrinosneutrinos
p,tap,tap,t i†jij
p,tap,tap,t i
†jij
p,tbp,tbp,t j†iij
p,tbp,tbp,t j
†iij
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
General Equations of MotionGeneral Equations of Motion
pqqqp3
3
FpFp
2
pt ),)(cos1(2
qdG2],L[G2,
p2M
i
pqqqp3
3
FpFp
2
pt ),)(cos1(2
qdG2],L[G2,
p2M
i
pqqqp3
3
FpFp
2
pt ),)(cos1(2
qdG2],L[G2,
p2M
i
pqqqp3
3
FpFp
2
pt ),)(cos1(2
qdG2],L[G2,
p2M
i
Usual matter effect withUsual matter effect with
nn00
0nn0
00nn
Lee
nn00
0nn0
00nn
Lee
• Vacuum oscillationsVacuum oscillations M is neutrino mass M is neutrino mass matrixmatrix
• Note opposite sign Note opposite sign betweenbetween neutrinos and neutrinos and antineutrinosantineutrinosNonlinear nu-nu effects are importantNonlinear nu-nu effects are importantwhen nu-nu interaction energy exceedswhen nu-nu interaction energy exceedstypical vacuum oscillation frequencytypical vacuum oscillation frequency(Do not compare with matter effect!)(Do not compare with matter effect!)
cos1nG2E2
mF
2
osc
cos1nG2E2
mF
2
osc
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Toy Supernova in “Single-Angle” Toy Supernova in “Single-Angle” ApproximationApproximation
BipolarOscillations
• 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)
Decline of oscillation amplitudeDecline of oscillation amplitudeexplained in pendulum analogyexplained in pendulum analogyby inreasing moment of inertiaby inreasing moment of inertia(Hannestad, Raffelt, Sigl & Wong(Hannestad, Raffelt, Sigl & Wong astro-ph/0608695)astro-ph/0608695)
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Collective SN neutrino oscillations 2006-2007Collective SN neutrino oscillations 2006-2007
““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
• Raffelt & Sigl, hep-ph/0701182Raffelt & Sigl, hep-ph/0701182• Esteban-Pretel, Pastor, Tomas,Esteban-Pretel, Pastor, Tomas, 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, arXiv:0705.1830, 0709.46410709.4641 • 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 Physik Kolloquium, 19. November 2007, RWTH Aachen
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Cosmic Diffuse Cosmic Diffuse SupernovaSupernova
Neutrino Background Neutrino Background (DSNB)(DSNB)
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Diffuse Background Flux of SN NeutrinosDiffuse Background Flux of SN Neutrinos
1 SNu ~ 4 L1 SNu ~ 4 L / L / L,B,B
Average neutrinoAverage neutrinoluminosity of galaxiesluminosity of galaxies~ photon luminosity~ photon luminosity
1 SNu 1 SNu == 1 SN / 10 1 SN / 101010 L Lsun,Bsun,B / 100 years / 100 years
LLsun,Bsun,B == 0.54 L 0.54 Lsunsun == 2 2 10103333 erg/serg/s
EE ~ 3 ~ 3 10105353 erg per core-collapse SN erg per core-collapse SN
For galaxies, averageFor galaxies, averagenuclear & gravitationalnuclear & gravitationalenergy release comparableenergy release comparable
• Photons come from nuclear energyPhotons come from nuclear energy
• Neutrinos from gravitational energyNeutrinos from gravitational energy
Present-day SN rate of ~ 1 SNu, extrapolated to the entire universe,Present-day SN rate of ~ 1 SNu, extrapolated to the entire universe,
corresponds to corresponds to ee flux of ~ 1 cm flux of ~ 1 cm22 s s11
Realistic flux is dominated by much larger early star-formation rateRealistic flux is dominated by much larger early star-formation rate Upper limit ~ 54 cmUpper limit ~ 54 cm22 s s11
[Kaplinghat et al., astro-ph/9912391][Kaplinghat et al., astro-ph/9912391] “ “Realistic estimate” ~ 10 cmRealistic estimate” ~ 10 cm22 s s11
[Hartmann & Woosley, Astropart. Phys. 7 (1997) 137][Hartmann & Woosley, Astropart. Phys. 7 (1997) 137] Measurement would tell us about early history of star formation Measurement would tell us about early history of star formation
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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 Physik Kolloquium, 19. November 2007, RWTH Aachen
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]
Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen
Aachen SkylineAachen Skyline
Looking forward to the next galactic supernova!
top related