Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen Title Title Georg Raffelt, Max-Planck-Institut für Georg Raffelt, Max-Planck-Institut für Physik, München Physik, München hysik Kolloquium, hysik Kolloquium, 19. 19. November 200 November 200 RWTH Aachen RWTH Aachen Exzellenz Exzellenz
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Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH AachenTitle Georg Raffelt, Max-Planck-Institut für Physik,
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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
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
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
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
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
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
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.
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
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]
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
• 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
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
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
• 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
Numerical simulationsNumerical simulations• Including multi-angle effectsIncluding multi-angle effects• Discovery of “spectral splits”Discovery of “spectral splits”
• 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
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