georg raffelt, max-planck-institut für physik, münchen physik kolloquium, 23. november 2007, tu...

Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 23. November 2007, TU Darmstadt

TitleTitle

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

TU Darmstadt, Physik Kolloquium, 23. November 2007TU Darmstadt, Physik Kolloquium, 23. November 2007

Neutrinos inNeutrinos inAstrophysics and CosmologyAstrophysics and Cosmology


Pauli’s Explanation of the Beta Decay Pauli’s Explanation of the Beta Decay Spectrum (1930)Spectrum (1930)

Niels Bohr:Niels Bohr:

Energy not conservedEnergy not conservedin the in the quantum domain?quantum domain?

Wolfgang PauliWolfgang Pauli(1900-1958)(1900-1958)

Nobel Prize 1945Nobel Prize 1945

““Neutron”Neutron”(1930)(1930)

““Neutron”Neutron”(1930)(1930)

““Neutrino”Neutrino”(E.Fermi)(E.Fermi)


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


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


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)


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 Neutrino DetectorSuper-Kamiokande Neutrino Detector

42 m42 m

39.3 39.3 mm


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



Solar Neutrino SpectrumSolar Neutrino Spectrum

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


BOREXINOBOREXINO

• Expected without flavor Expected without flavor oscillationsoscillations

75 75 ± 4 ± 4 c/100t/dc/100t/d• Expected with oscillationsExpected with oscillations

49 ± 4 49 ± 4 c/100t/dc/100t/d• BOREXINO result (August BOREXINO result (August

07)07)

47 ± 747 ± 7statstat ± 12 ± 12syssys c/100t/dc/100t/d

• 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


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


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 m11


Mass mMass m11

Mass mMass m22 >> m m11



Neutrino OscillationsNeutrino Oscillations

Mass mMass m11

Mass mMass m22 >> m m11Oscillation lengthOscillation length

21

22 mm

E4

21

22 mm

E4



Neutrino OscillationsNeutrino Oscillations

Oscillation lengthOscillation length

21

22 mm

E4

21

22 mm

E4



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 ??


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



Crab NebulaCrab Nebula



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


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


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”


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• 22 of 80 strings installed (2007)22 of 80 strings installed (2007)• Completion until 2011 foreseenCompletion until 2011 foreseen


Global Cosmic Ray SpectrumGlobal Cosmic Ray Spectrum


Core of the Galaxy NGC 4261 Core of the Galaxy NGC 4261



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


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,MeV15E

xe


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


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]


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)


TitleTitle

Dark Energy 73%Dark Energy 73% (Cosmological Constant)(Cosmological Constant)

NeutrinosNeutrinos 0.10.12%2%

DarkDark Matter 23%Matter 23%

Normal Matter 4%Normal Matter 4%(of this about 10%(of this about 10% luminous) luminous)



““Weighing” Neutrinos with KATRINWeighing” Neutrinos with KATRIN

• Sensitive to Sensitive to common mass scale mcommon mass scale m for all flavors because of small massfor all flavors because of small mass differences from oscillationsdifferences from oscillations• Best limit from Mainz und TroitskBest limit from Mainz und Troitsk m m << 2.2 eV (95% CL) 2.2 eV (95% CL)• KATRIN can reach KATRIN can reach 0.2 eV0.2 eV• Under constructionUnder construction• Data taking foreseen to begin in 2009Data taking foreseen to begin in 2009

http://www-ik.fzk.de/katrin/http://www-ik.fzk.de/katrin/


““KATRIN Approaching” (25 Nov 2006)KATRIN Approaching” (25 Nov 2006)


Cosmological Limit on Neutrino MassesCosmological Limit on Neutrino Masses

4.0eV94

mh2

4.0

eV94

mh2

Cosmic neutrino “sea”Cosmic neutrino “sea” ~ 112 cm~ 112 cm-3-3 neutrinos + anti-neutrinos per neutrinos + anti-neutrinos per flavor flavor

mm < 40 eV < 40 eV For allFor allstable flavorsstable flavors

A classic paper:A classic paper: Gershtein & ZeldovichGershtein & Zeldovich JETP Lett. 4 (1966) 120JETP Lett. 4 (1966) 120


Strukturbildung im UniversumStrukturbildung im Universum

SmoothSmooth StructuredStructured

Structure forms byStructure forms by gravitational instabilitygravitational instability of primordialof primordial density fluctuationsdensity fluctuations

A fraction of hot dark matter A fraction of hot dark matter suppresses small-scale structuresuppresses small-scale structure


Structure Formation with Hot Dark MatterStructure Formation with Hot Dark Matter

Troels Haugbølle, http://whome.phys.au.dk/~haugboelTroels Haugbølle, http://whome.phys.au.dk/~haugboel

Neutrinos with Neutrinos with mm = 6.9 eV = 6.9 eVStandard Standard CDM ModelCDM Model

Structure fromation simulated with Gadget codeStructure fromation simulated with Gadget codeCube size 256 Mpc at zero redshiftCube size 256 Mpc at zero redshift


Power Spectrum of Cosmic Density Power Spectrum of Cosmic Density FluctuationsFluctuations


Some Recent Cosmological Limits on Neutrino Some Recent Cosmological Limits on Neutrino MassesMassesmm/eV/eV(limit 95%CL)(limit 95%CL)

Data / PriorsData / Priors

Spergel et al. (WMAP) 2003Spergel et al. (WMAP) 2003 [astro-ph/0302209] [astro-ph/0302209] 0.690.69 WMAP-1, 2dF, HST, WMAP-1, 2dF, HST, 88

Hannestad 2003Hannestad 2003 [astro-ph/0303076][astro-ph/0303076]1.011.01 WMAP-1, CMB, 2dF, HSTWMAP-1, CMB, 2dF, HST

Crotty et al. 2004Crotty et al. 2004 [hep-ph/0402049][hep-ph/0402049]

1.01.00.60.6

WMAP-1, CMB, 2dF, SDSSWMAP-1, CMB, 2dF, SDSS& HST, SN& HST, SN

Hannestad 2004Hannestad 2004 [hep-ph/0409108][hep-ph/0409108] 0.650.65 WMAP-1, SDSS, SN Ia gold sample,WMAP-1, SDSS, SN Ia gold sample,

Ly-Ly- data from Keck sample data from Keck sample

Seljak et al. 2004Seljak et al. 2004 [[astro-ph/0407372]astro-ph/0407372]0.420.42 WMAP-1, SDSS, Bias,WMAP-1, SDSS, Bias,

Ly-Ly- data from SDSS sample data from SDSS sample

Spergel et al. 2006Spergel et al. 2006 [hep-ph/0409108][hep-ph/0409108] 0.680.68 WMAP-3, SDSS, 2dF, SN Ia, WMAP-3, SDSS, 2dF, SN Ia, 88

Seljak et al. 2006Seljak et al. 2006 [astro-ph/0604335][astro-ph/0604335]0.140.14 WMAP-3, CMB-small, SDSS, 2dF,WMAP-3, CMB-small, SDSS, 2dF,

SN Ia, BAO (SDSS), SN Ia, BAO (SDSS), Ly-Ly- (SDSS) (SDSS)

Hannestad et al. 2006Hannestad et al. 2006 [hep-ph/0409108][hep-ph/0409108] 0.300.30 WMAP-1, CMB-small, SDSS, 2dF,WMAP-1, CMB-small, SDSS, 2dF,

SN Ia, BAO (SDSS), SN Ia, BAO (SDSS), Ly-Ly- (SDSS) (SDSS)


Fermion Mass SpectrumFermion Mass Spectrum

1010 10010011 1010 10010011 1010 10010011 1010 10010011 1010 10010011 11meVmeV eVeV keVkeV MeVMeV GeVGeV TeVTeV

dd ss bbQuarks (Q = Quarks (Q = 1/3)1/3)

uu cc ttQuarks (Q = Quarks (Q = 2/3)2/3)

Charged Leptons (Q = Charged Leptons (Q = 1)1) ee

All flavorsAll flavors

33NeutrinosNeutrinos


Periodic System of Elementary ParticlesPeriodic System of Elementary Particles


2/32/3

cc

tt

Gravitation Gravitation

Weak InteractionWeak Interaction

Strong Int’n Strong Int’n

Electromagnetic Int’nElectromagnetic Int’n

1/3 1/3

ss

bb

1 1

0 0

11stst Family Family

22ndnd Family Family

33rdrd Family Family

uu dd ee ee

ChargeCharge 0 0

MatterMatter

Anti-QuarksAnti-QuarksAnti-LeptonsAnti-Leptons

2/32/31/3 1/3 0 0 1 1

eeee dd uu

ss

bb

cc

tt

Strong Int’nStrong Int’n

Electromagnetic Int’nElectromagnetic Int’n

AntimatterAntimatter

Why is there no antimatterWhy is there no antimatterin the Universe?in the Universe?

(Problem of „Baryogenesis”)(Problem of „Baryogenesis”)

0 0

ee

00

LeptonsLeptons Anti-LeptonsAnti-Leptons

„„Majorana Neutrinos”Majorana Neutrinos”are their ownare their ownantiparticlesantiparticles

Can explain baryogenesisCan explain baryogenesisby leptogenesisby leptogenesis


NeutrinosNeutrinosCharged LeptonsCharged Leptons

See-Saw Model for Neutrino MassesSee-Saw Model for Neutrino Masses

DiagonalizeDiagonalize

Lagrangian for Lagrangian for particle massesparticle masses massL massL .c.h .c.h

Dirac massesDirac masses from couplingfrom coupling to standardto standard Higgs field Higgs field

RLRL Ngeg RLRL Ngeg

HeavyHeavy Majorana Majorana masses masses

MMjj > 10 > 101010 GeV GeV

RcR2

1 MNN RcR2

1 MNN

R

LRL NMg

g0N

R

LRL NMg

g0N

R

L

22

RL NM0

0M

g

N

R

L

22

RL NM0

0M

g

N

Light Majorana massLight Majorana mass

Mg 22

Mg 22


See-Saw Model for Neutrino MassesSee-Saw Model for Neutrino Masses

R

L

22

RL NM0

0M

g

N

R

L

22

RL NM0

0M

g

N

Light Majorana massLight Majorana mass

Mg 22

Mg 22

N

ℓ

10101010 GeVGeV 11 GeVGeV 10101010

GeVGeV

ChargedChargedleptonsleptons

OrdinaryOrdinaryneutrinosneutrinos

HeavyHeavy““right-handed”right-handed”neutrinosneutrinos(no gauge(no gauge interactions)interactions)


EquilibriumEquilibriumabundance ofabundance ofheavy Majoranaheavy Majorananeutrinosneutrinos

W. Buchmüller & M. Plümacher: Neutrino masses and the baryon asymmetryW. Buchmüller & M. Plümacher: Neutrino masses and the baryon asymmetryInt. J. Mod. Phys. A15 (2000) 5047-5086Int. J. Mod. Phys. A15 (2000) 5047-5086

M. Fukugita & T. Yanagida:M. Fukugita & T. Yanagida: Baryogenesis without GrandBaryogenesis without Grand UnificationUnification Phys. Lett. B 174 (1986) 45 Phys. Lett. B 174 (1986) 45

Leptogenesis by Out-of-Equilibrium DecayLeptogenesis by Out-of-Equilibrium Decay


Real abundanceReal abundancedetermined bydetermined bydecay ratedecay rate

CreatedCreatedlepton-numberlepton-numberabundanceabundance


Real abundanceReal abundancedetermined bydetermined bydecay ratedecay rate

CP-violating decays byCP-violating decays by interference of tree-levelinterference of tree-level with one-loop diagramwith one-loop diagram

8M2

Decay g 8M2

Decay g


Leptogenesis by Majorana Neutrino DecaysLeptogenesis by Majorana Neutrino Decays

In see-saw models for neutrino masses, out-of-equilibriumIn see-saw models for neutrino masses, out-of-equilibrium decays of right-handed heavy Majorana neutrinos providedecays of right-handed heavy Majorana neutrinos provide source for CP- and L-violationsource for CP- and L-violation

Cosmological evolutionCosmological evolution• B = L = 0 early onB = L = 0 early on• Thermal freeze-out of heavy Majorana neutrinosThermal freeze-out of heavy Majorana neutrinos• Out-of-equilibrium CP-violating decay creates net LOut-of-equilibrium CP-violating decay creates net L• Shift L excess into B by sphaleron effectsShift L excess into B by sphaleron effects

Sufficient deviation Sufficient deviation from equilibrium from equilibrium distribution of heavy distribution of heavy Majorana neutrinos at Majorana neutrinos at freeze-outfreeze-out

Limits Limits ononYukawaYukawacouplincouplingsgs

Limits Limits ononmasses masses ofofordinarordinaryyneutrinneutrinososRequires Majorana neutrino masses below 0.1 eVRequires Majorana neutrino masses below 0.1 eV

Buchmüller, Di Bari & Plümacher, hep-ph/0209301 & hep-ph/0302092Buchmüller, Di Bari & Plümacher, hep-ph/0209301 & hep-ph/0302092


TitleTitle

Dark Energy 73%Dark Energy 73% (Cosmological Constant)(Cosmological Constant)

NeutrinosNeutrinos 0.10.12%2%

DarkDark Matter 23%Matter 23%

Normal Matter 4%Normal Matter 4%(of this about 10%(of this about 10% luminous) luminous)

Massive neutrinos canMassive neutrinos canexplain presence of explain presence of mattermatterby leptogenesis by leptogenesis mechanismmechanism



Killing Two Birds with One StoneKilling Two Birds with One Stone

See-Saw mechanism explainsSee-Saw mechanism explains• Small neutrino massesSmall neutrino masses• Baryon asymmetry of theBaryon asymmetry of the universe by leptogenesisuniverse by leptogenesis


Leptogenesis by Majorana Neutrino DecaysLeptogenesis by Majorana Neutrino Decays

A classic paper


Leptogenesis as a Research TopicLeptogenesis as a Research Topic

Citation of Fukugita & Yanagida, PLB 174 (1986) 45Citation of Fukugita & Yanagida, PLB 174 (1986) 45or “leptogenesis” in title (SPIRES data base)or “leptogenesis” in title (SPIRES data base)

0

20

40

60

80

100

120

140

160

180

1986 1988 1990 1992 1994 1996 1998 2000 2002 2004 2006


Portion of the Hubble Ultra Deep Field

Portion of the Hubble Ultra Deep Field

Astrophysics & Cosmology

Astrophysics & Cosmology

Cosm

ic Rays

Cosmic

Rays

E

lem

en

tary

Part

icle

Ph

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s

Ele

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Part

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Gamow & Schoenberg 2Gamow & Schoenberg 2


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)


Geo NeutrinosGeo Neutrinos

Predicted geo neutrino fluxPredicted geo neutrino flux

Reactor backgroundReactor background

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


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

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bDestructionDestructionoperators foroperators for(anti)neutrinos(anti)neutrinos

0

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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


General Equations of MotionGeneral Equations of Motion

pqqqp3

3

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2

pt ),)(cos1(2

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Usual matter effect withUsual matter effect with

nn00

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nn00

0nn0

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• 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

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cos1nG2E2

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2

osc


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)


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


SN 1006SN 1006

Looking forward to the next galactic supernovaLooking forward to the next galactic supernova

http://antwrp.gsfc.nasa.gov/apod/ap060430.htmlhttp://antwrp.gsfc.nasa.gov/apod/ap060430.html


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


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


Neutrinos in Astrophysics and CosmologyNeutrinos in Astrophysics and Cosmology

Neutrinos Neutrinos responsibleresponsible for ordinaryfor ordinary astrophysicalastrophysical andand cosmologicalcosmological phenomenaphenomena

• Dominant radiation component in the early universeDominant radiation component in the early universe• Crucial role in big-bang nucleosynthesisCrucial role in big-bang nucleosynthesis• Dark-matter component (but subdominant)Dark-matter component (but subdominant)• May be responsible for baryonic matter in theMay be responsible for baryonic matter in the universe (leptogenesis)universe (leptogenesis)• Important (sometimes dominant) cooling agent of starsImportant (sometimes dominant) cooling agent of stars• May trigger supernova explosionsMay trigger supernova explosions• May be crucial for r-process nucleosynthesisMay be crucial for r-process nucleosynthesis

HeavenlyHeavenly laboratorieslaboratories for newfor new particleparticle physicsphysics phenomenaphenomena

• Cosmological limit (future detection?) of nu mass scaleCosmological limit (future detection?) of nu mass scale• Flavor oscillations of solar and atmospheric neutrinosFlavor oscillations of solar and atmospheric neutrinos• Neutrino oscillations from a future galactic supernovaNeutrino oscillations from a future galactic supernova• Limits on “exotic” neutrino propertiesLimits on “exotic” neutrino properties (dipole moments, right-handed interactions, decays,(dipole moments, right-handed interactions, decays, flavor-violating neutral currents, sterile nus, …)flavor-violating neutral currents, sterile nus, …)

Neutrinos asNeutrinos as astrophysicalastrophysical messengersmessengers

• Look into the solar interior (“measure” temperature)Look into the solar interior (“measure” temperature)• Watch stellar collapse directlyWatch stellar collapse directly• Neutrinos from all cosmological supernovaeNeutrinos from all cosmological supernovae• Astrophysical accelerators for cosmic raysAstrophysical accelerators for cosmic rays• Annihilation signature for neutralino dark matterAnnihilation signature for neutralino dark matter


Hot dark matter ruled out in 1983Hot dark matter ruled out in 1983

1000 particle simulation [Frenk, White & Davis, ApJ 271 (1983) 417]1000 particle simulation [Frenk, White & Davis, ApJ 271 (1983) 417]

The coherence length of the neutrino distribution […] is too largeThe coherence length of the neutrino distribution […] is too largeto be consistent with the observed clustering scale of galaxies […]to be consistent with the observed clustering scale of galaxies […]The conventional neutrino-dominated picture appears to be ruledThe conventional neutrino-dominated picture appears to be ruledout. White, Frenk & Davis, ApJ 274 (1983) L1.out. White, Frenk & Davis, ApJ 274 (1983) L1.

georg raffelt, max-planck-institut für physik, münchen physik kolloquium, 23. november 2007, tu...

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