Georg Raffelt, Max-Planck-Institut für Physik, München25ème Journée Thématique de lIPN, 3 Juin 2008, Orsay SN 1006 Georg Raffelt, Max-Planck-Institut für.

Georg Raffelt, Max-Planck-Institut für Physik, München 25ème Journée Thématique de l’IPN, 3 Juin 2008, Orsay

SN 1006SN 1006

Georg Raffelt, Max-Planck-Institut für Physik, Georg Raffelt, Max-Planck-Institut für Physik, MünchenMünchen

2525èmeème Journée Thématique de l’IPN, 3 Juin 2008, Orsay Journée Thématique de l’IPN, 3 Juin 2008, Orsay

Frontiers ofFrontiers ofLow-Energy Neutrino Astronomy:Low-Energy Neutrino Astronomy:Earth, Sun and SupernovaeEarth, Sun and Supernovae


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)


Neutrinos from nuclearNeutrinos from nuclearreactions:reactions:

Energies 1Energies 120 MeV20 MeV

““Beam dump neutrinos”Beam dump neutrinos”• High-energy protons hitHigh-energy protons hit matter or photonsmatter or photons

• Produce secondary Produce secondary

• Neutrinos from pionNeutrinos from pion decay decay

ee ee

• Energies Energies ≫≫ GeV GeV

Quasi thermal sourcesQuasi thermal sources

Supernova: T ~ few MeVSupernova: T ~ few MeV

Big-Bang Neutrinos:Big-Bang Neutrinos:Very small energies todayVery small energies today(cosmic red shift)(cosmic red shift)

Like matter todayLike matter today



Low-energyLow-energyneutrino astronomyneutrino astronomy(including geo-neutrinos)(including geo-neutrinos)Energies ~ 1Energies ~ 150 MeV50 MeV

High-energyHigh-energyneutrino astronomyneutrino astronomy

Closely related toClosely related tocosmic-ray physicscosmic-ray physics

Long-baselineLong-baselineneutrino oscillationneutrino oscillationexperiments withexperiments with• Reactor neutrinosReactor neutrinos• Neutrino beams fromNeutrino beams from acceleratorsaccelerators



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


Bethe’s Classic Paper on Nuclear Reactions in Bethe’s Classic Paper on Nuclear Reactions in StarsStars

No neutrinosNo neutrinosfrom nuclear from nuclear

reactionsreactionsin 1938 … in 1938 …


Gamow & Schoenberg, Phys. Rev. 58:1117 Gamow & Schoenberg, Phys. Rev. 58:1117 (1940)(1940)


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


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--


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


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)



Super-Kamiokande: Sun in the Light of Super-Kamiokande: Sun in the Light of NeutrinosNeutrinos



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”


John BahcallJohn Bahcall1934 1934 20052005

Raymond Davis Jr.Raymond Davis Jr.1914 1914 2006 2006

Missing Neutrinos from the SunMissing Neutrinos from the Sun

HomestakeHomestake

ChlorineChlorine

77BeBe

88BB

CNOCNO

Measurement (1970Measurement (1970 –– 1995)1995)

Calculation of expectedCalculation of expectedexperimental countingexperimental countingrate from variousrate from varioussource reactionssource reactions


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


Missing Neutrinos from the SunMissing Neutrinos from the Sun

HomestakeHomestake

77BeBe

88BB

CNOCNO

ChlorineChlorine

Gallex/GNOGallex/GNOSAGESAGE

CNOCNO

77BeBe

pppp

88BB

GalliumGallium

Electron-Neutrino DetectorsElectron-Neutrino Detectors

(Super-)(Super-)KamiokandeKamiokande

88BB

WaterWateree++ ee ee++ ee

SNOSNO

88BB

ee++ dd pp ++ pp ++ eeHeavy WaterHeavy Water

88BB

++ dd pp ++ nn ++ Heavy WaterHeavy Water

All FlavorsAll Flavors

SNOSNO

88BB

WaterWater + e+ e + e+ e


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 ??


Solar Neutrino SpectrumSolar Neutrino Spectrum

7-Be line measured7-Be line measuredby Borexino (2007)by Borexino (2007)


Solar Neutrino Spectroscopy with Solar Neutrino Spectroscopy with BOREXINOBOREXINO

• Neutrino electron scatteringNeutrino electron scattering• Liquid scintillator technologyLiquid scintillator technology (~ 300 tons)(~ 300 tons)• Low energy thresholdLow energy threshold (~ 60 keV)(~ 60 keV)• Online since 16 May 2007Online since 16 May 2007


• Expected without flavor Expected without flavor oscillationsoscillations75 75 ± 4 ± 4 counts/100t/dcounts/100t/d

• Expected with oscillationsExpected with oscillations49 ± 4 49 ± 4 counts/100t/dcounts/100t/d

• BOREXINO result (May BOREXINO result (May 2008)2008)

49 ± 349 ± 3statstat ± 4 ± 4syssys cnts/100t/dcnts/100t/d arXiv:0805.3843 (25 May 2008)arXiv:0805.3843 (25 May 2008)


Next Steps in BorexinoNext Steps in Borexino

• Collect more statistics of Beryllium lineCollect more statistics of Beryllium line

• Seasonal variation of rateSeasonal variation of rate (Earth orbit eccentricity)(Earth orbit eccentricity)

• Measure neutrinos from the CNO reaction chainMeasure neutrinos from the CNO reaction chain• Information about solar metal abundanceInformation about solar metal abundance

Measure geo-neutrinos Measure geo-neutrinos (from natural radioactivity in the Earth crust)(from natural radioactivity in the Earth crust) Approx. 7Approx. 717 events/year17 events/year Main background: Reactors ~ 20 events/yearMain background: Reactors ~ 20 events/year


Geo Neutrinos: Why and What?Geo Neutrinos: Why and What?

We know surprisingly little aboutWe know surprisingly little aboutthe interior of the Earth:the interior of the Earth:

• Deepest bore hole ~ 12 kmDeepest bore hole ~ 12 km• Samples from the crust areSamples from the crust are available for chemical analysisavailable for chemical analysis (e.g. vulcanoes)(e.g. vulcanoes)• Seismology reconstructs densitySeismology reconstructs density profile throughout the Earthprofile throughout the Earth• Heat flow from measuredHeat flow from measured temperature gradients 30temperature gradients 3044 TW44 TW (BSE canonical model, based on(BSE canonical model, based on cosmochemical arguments,cosmochemical arguments, predicts ~ 19 TW from crust and predicts ~ 19 TW from crust and mantle, none from core)mantle, none from core)

• Neutrinos escape freelyNeutrinos escape freely

• Carry information about chemical composition, radioactive heat production,Carry information about chemical composition, radioactive heat production, or even a putative natural reactor at the coreor even a putative natural reactor at the core


Expected Geo Neutrino FluxesExpected Geo Neutrino Fluxes

S. Dye, Talk 5/25/2006S. Dye, Talk 5/25/2006BaltimoreBaltimore


Geo NeutrinosGeo Neutrinos

Predicted geo neutrino fluxPredicted geo neutrino flux

Reactor backgroundReactor background

KamLAND scintillator detector (1 kton)KamLAND scintillator detector (1 kton)


Kamland Observation of GeoneutrinosKamland Observation of Geoneutrinos

• First tentative observation of geoneutrinosFirst tentative observation of geoneutrinos at Kamland in 2005 (~ 2 sigma effect)at Kamland in 2005 (~ 2 sigma effect)• Very difficult because of large backgroundVery difficult because of large background of reactor neutrinosof reactor neutrinos (is main purpose for neutrino oscillations)(is main purpose for neutrino oscillations)


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



Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A



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


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



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



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


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


Do Neutrinos Gravitate?Do Neutrinos Gravitate?

Neutrinos arrive a few hours earlier than photons Neutrinos arrive a few hours earlier than photons Early warning (SNEWS) Early warning (SNEWS)SN 1987A: Transit time for photons and neutrinos equal to within ~ 3hSN 1987A: Transit time for photons and neutrinos equal to within ~ 3h

Equal within ~ 1 Equal within ~ 1 4 4 101033

Shapiro time delay for particles moving in a Shapiro time delay for particles moving in a gravitational potential gravitational potential

Longo, PRL 60:173,1988Longo, PRL 60:173,1988Krauss & Tremaine, PRL 60:176,1988Krauss & Tremaine, PRL 60:176,1988

• Proves directly that neutrinos respond to gravity in the usual wayProves directly that neutrinos respond to gravity in the usual way because for photons gravitational lensing already proves this pointbecause for photons gravitational lensing already proves this point

• Cosmological limits Cosmological limits NN ≲≲ 1 much worse test of neutrino gravitation 1 much worse test of neutrino gravitation

• Provides limits on parameters of certain non-GR theories of gravitationProvides limits on parameters of certain non-GR theories of gravitation

months51dt)]t(r[U2t BAShapiro months51dt)]t(r[U2t BAShapiro


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


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



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)


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


IceCube Neutrino Telescope at the South PoleIceCube Neutrino Telescope at the South Pole

• 1 km1 km33 antarctic ice, instrumented antarctic ice, instrumented with 4800 photomultiplierswith 4800 photomultipliers• 40 of 80 strings installed (2008)40 of 80 strings installed (2008)• Completion until 2011 foreseenCompletion until 2011 foreseen


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


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


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


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


Collective Effects in Neutrino Flavor Collective Effects in Neutrino Flavor OscillationsOscillationsCollapsed supernova core or accretion torus ofCollapsed supernova core or accretion torus ofmerging neutron stars:merging neutron stars:

• Neutrino flux very dense: Up to 10Neutrino flux very dense: Up to 103535 cm cm3 3

• Neutrino-neutrino interaction energy Neutrino-neutrino interaction energy much larger than vacuum oscillation frequencymuch larger than vacuum oscillation frequency• Large “matter effect” of neutrinos on eachLarge “matter effect” of neutrinos on each otherother• Non-linear oscillation effectsNon-linear oscillation effects

• Assume 80% anti-neutrinosAssume 80% anti-neutrinos• Vacuum oscillation frequencyVacuum oscillation frequency

= 0.3 km= 0.3 km11

• Neutrino-neutrino interaction Neutrino-neutrino interaction energy at nu sphere (r = 10 km)energy at nu sphere (r = 10 km)

= 0.3= 0.3101055 km km11

• Falls off approximately as Falls off approximately as rr44

(geometric flux dilution and nus(geometric flux dilution and nus become more co-linear)become more co-linear)


Spectral Split (Stepwise Spectral Swapping)Spectral Split (Stepwise Spectral Swapping)

Fogli, Lisi, Marrone & Mirizzi, arXiv:0707.1998Fogli, Lisi, Marrone & Mirizzi, arXiv:0707.1998

Initial fluxesInitial fluxesat nu sphereat nu sphere

AfterAftercollectivecollectivetrans-trans-formationformation

For explanation seeFor explanation see

Raffelt & SmirnovRaffelt & Smirnov arXiv:0705.1830arXiv:0705.1830 arXiv:0709.4641arXiv:0709.4641

Duan, Fuller,Duan, Fuller,Carlson & QianCarlson & Qian arXiv:0706.4293arXiv:0706.4293 arXiv:0707.0290arXiv:0707.0290


Mass Hierarchy at Extremely Small Theta-13Mass Hierarchy at Extremely Small Theta-13

Dasgupta, Dighe & Mirizzi, arXiv:0802.1481Dasgupta, Dighe & Mirizzi, arXiv:0802.1481

Ratio of spectra inRatio of spectra intwo water Cherenkovtwo water Cherenkovdetectors (0.4 Mton),detectors (0.4 Mton),one shadowed by theone shadowed by theEarth, the other notEarth, the other not

Using Earth matter effects to diagnose transformationsUsing Earth matter effects to diagnose transformations


Collective SN neutrino oscillations 2006-2008 Collective SN neutrino oscillations 2006-2008 (I)(I)

““Bipolar” collective transformationsBipolar” collective transformationsimportant, even for dense matterimportant, even for dense matter

• Duan, Fuller & Qian Duan, Fuller & Qian astro-ph/0511275astro-ph/0511275

Numerical simulationsNumerical simulations• Including multi-angle effectsIncluding multi-angle effects• Discovery of “spectral splits”Discovery of “spectral splits”

• Duan, Fuller, Carlson & QianDuan, Fuller, Carlson & Qian astro-ph/0606616, 0608050astro-ph/0606616, 0608050

• Pendulum in flavor spacePendulum in flavor space• Collective pair annihilationCollective pair annihilation• Pure precession modePure precession mode

• Hannestad, Raffelt, Sigl & WongHannestad, Raffelt, Sigl & Wong astro-ph/0608695astro-ph/0608695• Duan, Fuller, Carlson & QianDuan, Fuller, Carlson & Qian astro-ph/0703776astro-ph/0703776

Self-maintained coherenceSelf-maintained coherencevs. self-induced decoherencevs. self-induced decoherencecaused by multi-angle effectscaused by multi-angle effects

• Sawyer, hep-ph/0408265, 0503013 Sawyer, hep-ph/0408265, 0503013 • Raffelt & Sigl, hep-ph/0701182Raffelt & Sigl, hep-ph/0701182• Esteban-Pretel, Pastor, Tomàs,Esteban-Pretel, Pastor, Tomàs, Raffelt & Sigl, arXiv:0706.2498Raffelt & Sigl, arXiv:0706.2498

Theory of “spectral splits”Theory of “spectral splits”in terms of adiabatic evolution inin terms of adiabatic evolution inrotating framerotating frame

• Raffelt & Smirnov,Raffelt & Smirnov, arXiv:0705.1830, 0709.4641 arXiv:0705.1830, 0709.4641 • Duan, Fuller, Carlson & QianDuan, Fuller, Carlson & Qian arXiv:0706.4293, 0707.0290 arXiv:0706.4293, 0707.0290

Independent numerical simulationsIndependent numerical simulations • Fogli, Lisi, Marrone & MirizziFogli, Lisi, Marrone & Mirizzi arXiv:0707.1998 arXiv:0707.1998


Collective SN neutrino oscillations 2006-2008 Collective SN neutrino oscillations 2006-2008 (II)(II)

Second-order mu-tau refractive effectSecond-order mu-tau refractive effectimportant in three-flavor contextimportant in three-flavor context

• Esteban-Pretel, Pastor, Tomàs,Esteban-Pretel, Pastor, Tomàs, Raffelt & Sigl, arXiv:0712.1137Raffelt & Sigl, arXiv:0712.1137

Three-flavor effects in O-Ne-Mg SNeThree-flavor effects in O-Ne-Mg SNeon neutronization burston neutronization burst(MSW-prepared spectral double split)(MSW-prepared spectral double split)

• Duan, Fuller, Carlson & Qian,Duan, Fuller, Carlson & Qian, arXiv:0710.1271arXiv:0710.1271• Dasgupta, Dighe, Mirrizzi & Raffelt,Dasgupta, Dighe, Mirrizzi & Raffelt, arXiv:0801.1660arXiv:0801.1660

Theory of three-flavor collectiveTheory of three-flavor collectiveoscillationsoscillations

• Dasgupta & Dighe,Dasgupta & Dighe, arXiv:0712.3798arXiv:0712.3798

Identifying the neutrino mass hierarchyIdentifying the neutrino mass hierarchyat extremely small Theta-13at extremely small Theta-13

• Dasgupta, Dighe & Mirizzi,Dasgupta, Dighe & Mirizzi, arXiv:0802.1481arXiv:0802.1481

Formulation for non-sphericalFormulation for non-sphericalgeometrygeometry

• Dasgupta, Dighe, Mirizzi & RaffeltDasgupta, Dighe, Mirizzi & Raffelt arXiv:0805.3300arXiv:0805.3300

Many theoretical questions for this neutrino many-body systemMany theoretical questions for this neutrino many-body systemremain unresolvedremain unresolved !!


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.


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


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]


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


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)


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, München25ème Journée Thématique de lIPN, 3 Juin 2008, Orsay SN 1006 Georg Raffelt, Max-Planck-Institut für.

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