Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Topical Seminar on Frontiers of Particle Physics 2002: NeutrinosTopical Seminar on Frontiers of Particle Physics 2002: Neutrinos and Cosmologyand CosmologyYun HuYun Hu Holiday Resort of MiHoliday Resort of Mi YunYun, Beijing, China (20, Beijing, China (20--25 August 2002)25 August 2002)
Neutrino AstrophysicsGeorg G. Raffelt
Max-Planck-Institut für Physik, München, Germany
Neutrino AstrophysicsGeorg G. Raffelt
Max-Planck-Institut für Physik, München, Germany
Lecture I:Lecture I:Physics with SupernovaePhysics with Supernovae
Lecture II:Lecture II:Cosmological NeutrinosCosmological Neutrinos
Lecture II:Lecture II:Cosmological NeutrinosCosmological Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Status of Evidence for Neutrino OscillationsStatus of Evidence for Neutrino Oscillations
AtmosphericAtmospheric SolarSolar LSNDLSNDSystemSystem
τµ ν→ν τµ ν→ν µτν→νe µτν→νe eν→νµ eν→νµChannelChannel
StatusStatus EstablishedEstablished EstablishedEstablished UnconfirmedUnconfirmed
Mutually inconsistent with 3 massMutually inconsistent with 3 mass eigenstateseigenstates
TestTest Long Baseline (K2K)Long Baseline (K2K) KamLANDKamLAND 2002 ?2002 ? MiniBooNEMiniBooNE 2004 ?2004 ?
Three massThree mass eigenstateseigenstates withwithmm11 << m<< m22 << m<< m33 ~ 50~ 50 meVmeV (hierarchical)(hierarchical)mm11 ~ m~ m22 ~ m~ m33 >> 50>> 50 meVmeV (degenerate)(degenerate)
SimplestSimplestinterpreinterpre--tationtation
ExperimentalExperimentalFlukeFluke
θ2sin2 θ2sin2 0.90.9−−11 0.20.2−−0.60.6 0.0010.001−−0.030.03
22 eV/mδ 22 eV/mδ LMALMA 0.20.2--22310)45.1( −×− 410)22.0( −×−
What is the absolute neutrino mass scaleWhat is the absolute neutrino mass scale mmνν??
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Lecture II: Cosmological NeutrinosLecture II: Cosmological Neutrinos
Neutrino Dark Matter and Neutrino Dark Matter and Cosmic Structure FormationCosmic Structure FormationNeutrino Dark Matter and Neutrino Dark Matter and Cosmic Structure FormationCosmic Structure Formation
Neutrino Chemical Potentials,Neutrino Chemical Potentials,BigBig--BangBang NucleosynthesisNucleosynthesis,,and Flavor Oscillationsand Flavor Oscillations
HighestHighest--Energy Cosmic Rays Energy Cosmic Rays and the Cosmic Neutrino Seaand the Cosmic Neutrino Sea
Massive Neutrinos and the Massive Neutrinos and the Cosmic Baryon AsymmetryCosmic Baryon Asymmetry
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Cosmological Limit on Neutrino MassesCosmological Limit on Neutrino Masses
Cosmic neutrino “sea”Cosmic neutrino “sea” ~ 112 cm~ 112 cm--33 neutrinos + antineutrinos + anti--neutrinos per flavor neutrinos per flavor
4.0eV94
mh2 <=Ω ∑
νν 4.0
eV94m
h2 <=Ω ∑ν
ν mmνν < 40 < 40 eVeV For allFor allstable flavorsstable flavors
A classic paper:A classic paper:GershteinGershtein & & ZeldovichZeldovichJETP JETP LettLett. 4 (1966) 120. 4 (1966) 120
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
FermionFermion Mass SpectrumMass Spectrum
Cosmological limit on all Cosmological limit on all stable flavorsstable flavors
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Weakly Interacting Particles as Dark MatterWeakly Interacting Particles as Dark Matter
Almost 30 years ago,Almost 30 years ago,beginnings of the idea ofbeginnings of the idea ofweakly interacting particlesweakly interacting particles(neutrinos) as dark matter(neutrinos) as dark matter
Massive neutrinos are noMassive neutrinos are nolonger a good candidatelonger a good candidate(hot dark matter)(hot dark matter)
However, the idea ofHowever, the idea ofweakly interacting massiveweakly interacting massiveparticles as dark matterparticles as dark matteris now standardis now standard
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
What is wrong with neutrino dark matter?What is wrong with neutrino dark matter?
Maximum mass density of aMaximum mass density of a FermiFermi gasgasρρmaxmax = = mmνν nnmaxmax = = mmνν ppmaxmax
33/3/3ππ2 2 = = mmνν ((mmννvvescapeescape))33/3/3ππ22
More restrictive from dwarf galaxiesMore restrictive from dwarf galaxiesmmνν > 100 > 100 –– 200 200 eVeV
Galactic Phase Space (“Galactic Phase Space (“TremaineTremaine--GunnGunn--Limit”)Limit”)
mmνν > 20> 20 –– 40 40 eVeV SpiralSpiralgalaxiesgalaxies
•• NusNus are “Hot Dark Matter”are “Hot Dark Matter”•• Ruled out Ruled out by structure formationby structure formation
Neutrino Free Streaming (Neutrino Free Streaming (CollisionlessCollisionless Phase Mixing)Phase Mixing)
•• AtAt TT << 11 MeVMeV neutrinoneutrino scatteringscattering inin earlyearly universeuniverse ineffectiveineffective•• Stream freely untilStream freely until nonrelativisticnonrelativistic•• Wash out density contrasts on small scales Wash out density contrasts on small scales
NeutrinosNeutrinosNeutrinosNeutrinos
OverOver--densitydensity
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Formation of StructureFormation of Structure
Numerical Simulation MaxNumerical Simulation Max--PlanckPlanck--Institut für AstrophysikInstitut für Astrophysik,, GarchingGarching
SmoothSmooth StructuredStructured
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
COBE Sky Map of the CMBR TemperatureCOBE Sky Map of the CMBR Temperature
T = 2.728 K (uniform on the sky)T = 2.728 K (uniform on the sky)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
COBE Sky Map of the CMBR TemperatureCOBE Sky Map of the CMBR Temperature
T = 2.728 K (uniform on the sky)T = 2.728 K (uniform on the sky)Dynamical rangeDynamical range ∆∆T = 3.353T = 3.353 mKmK
Dipole temperature distribution from Doppler effect due to Dipole temperature distribution from Doppler effect due to our motion relative to the cosmic frameour motion relative to the cosmic frame
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
COBE Sky Map of the CMBR TemperatureCOBE Sky Map of the CMBR Temperature
T = 2.728 K (uniform on the sky)T = 2.728 K (uniform on the sky)Dynamical rangeDynamical range ∆∆T = 3.353T = 3.353 mKmK
Dipole temperature distribution from Doppler effect due to Dipole temperature distribution from Doppler effect due to Dynamical rangeDynamical range ∆∆T = 18T = 18 µµKK
Primordial temperature fluctuationsPrimordial temperature fluctuationsour motion relative to the cosmic frameour motion relative to the cosmic frame
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Last Scattering SurfaceLast Scattering Surface
1133
202010
0010
0015
0015
00RedshiftRedshift zz
Here & Here & NowNow
HorizonHorizon
ΘΘ
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Power Spectrum of CMBR Temperature FluctuationsPower Spectrum of CMBR Temperature FluctuationsSky map of CMBR temperatureSky map of CMBR temperature
fluctuationsfluctuations
( ) ( )T
T,T, −ϕθ=ϕθ∆( ) ( )
TT,T, −ϕθ
=ϕθ∆
Multipole expansionMultipole expansion
( ) ( )ϕθ=ϕθ∆ ∑ ∑∞
= −=,Ya, m
0 mm l
l
l
ll( ) ( )ϕθ=ϕθ∆ ∑ ∑
∞
= −=,Ya, m
0 mm l
l
l
ll
Angular power spectrumAngular power spectrum
∑−=
∗∗+
==l
llllll
l mmmmm aa
121aaC ∑
−=
∗∗+
==l
llllll
l mmmmm aa
121aaC
Multipole Multipole RR
RR ((RR ++
11 ) ) CC
RR//22 ππ
Acoustic PeaksAcoustic PeaksAcoustic Peaks
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Multiple Peaks in CMBR Angular Power SpectrumMultiple Peaks in CMBR Angular Power Spectrum
CBICBI
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
A Slice of the UniverseA Slice of the Universe
Cosmic Cosmic “Stick Man”“Stick Man”
~ 185~ 185 Mpc
Mpc
Galaxy distribution from theGalaxy distribution from the CfA redshiftCfA redshift surveysurvey[[ApJApJ 302 (1986) L1]302 (1986) L1]
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
LasLas Campanas RedshiftCampanas Redshift SurveySurvey
~ 800~ 800
MpcMpc
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
2dF Galaxy2dF Galaxy RedshiftRedshift Survey (15 May 2002)Survey (15 May 2002)
~ 1300
~ 1300MpcMpc
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
2dF Galaxy2dF Galaxy RedshiftRedshift SurveySurvey
Animations from 2dFGRS Homepage http://www.Animations from 2dFGRS Homepage http://www.msomso..anuanu..eduedu.au/2dFGRS/.au/2dFGRS/
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Power Spectrum of Density FluctuationsPower Spectrum of Density Fluctuations
Field of density fluctuationsField of density fluctuations
ρδρ
=δ)x()x(
ρδρ
=δ)x()x(
GaussianGaussian random fieldrandom fieldfully characterizedfully characterizedby power spectrumby power spectrum
Fourier transformFourier transform
)x(exd)k( xik3 δ=δ ⋅−∫ )x(exd)k( xik3 δ=δ ⋅−∫
Power spectrum essentially square ofPower spectrum essentially square ofFourier transformFourier transform
with the delta functionwith the delta function( ) ( ) )k(Pkkˆ2)k()k( 3 ′−δπ=′δδ ( ) ( ) )k(Pkkˆ2)k()k( 3 ′−δπ=′δδ
δδ
Power spectrum is Fourier transformPower spectrum is Fourier transformof twoof two--point correlation functionpoint correlation function
where where ( )
)k(Pe2
kd)x()x()x( xik3
312
⋅∫π
=δδ=ξ( )
)k(Pe2
kd)x()x()x( xik3
312
⋅∫π
=δδ=ξ
12 xxx −= 12 xxx −=
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Fitting the Cosmological Model Fitting the Cosmological Model -- NeutrinosNeutrinos
Ionization parameterIonization parameter
CurvatureCurvature
Cosmological constantCosmological constant
Dark Matter (Dark Matter (ΩΩMMhh22))
Baryons (Baryons (ΩΩBBhh22))
Neutrino DM fractionNeutrino DM fraction
Scalar powerScalar power--law indexlaw index
Tensor powerTensor power--law indexlaw index
Scalar AmplitudeScalar Amplitude
Tensor AmplitudeTensor Amplitude
Biasing parameterBiasing parameter
Hubble constantHubble constant
Max Tegmark, www.hep.upenn.edu/~max/concordance.html
MaxMax TegmarkTegmark, , www.www.hephep..upennupenn..eduedu//~max/concordance.html~max/concordance.html
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Fitting the Cosmological Model Fitting the Cosmological Model -- NeutrinosNeutrinos
Ionization parameterIonization parameter
CurvatureCurvature
Cosmological constantCosmological constant
Dark Matter (Dark Matter (ΩΩMMhh22))
Baryons (Baryons (ΩΩBBhh22))
Neutrino DM fractionNeutrino DM fraction
Scalar powerScalar power--law indexlaw index
Tensor powerTensor power--law indexlaw index
Scalar AmplitudeScalar Amplitude
Tensor AmplitudeTensor Amplitude
Biasing parameterBiasing parameter
Hubble constantHubble constant
Max Tegmark, www.hep.upenn.edu/~max/concordance.html
MaxMax TegmarkTegmark, , www.www.hephep..upennupenn..eduedu//~max/concordance.html~max/concordance.html
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Neutrino Mass Limit from 2dF Galaxy SurveyNeutrino Mass Limit from 2dF Galaxy Survey
ElgaroyElgaroy et al.,et al.,astroastro--ph/0204152ph/0204152
ΩΩνν = 0.01= 0.01
ΩΩνν = 0= 0
ΩΩνν = 0.05= 0.05
ΣΣ mmνν < 2.2< 2.2 eVeVat 95% CLat 95% CL
For a similar limitFor a similar limitbased on the 2dFbased on the 2dFdata see data see HannestadHannestadastroastro--ph/0205223ph/0205223
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Matter Inventory of the UniverseMatter Inventory of the Universe
Dark Energy ~ 70%Dark Energy ~ 70%(Cosmological Constant)(Cosmological Constant)
Dark MatterDark Matter~ 25%~ 25%
Baryonic Matter ~ 5%Baryonic Matter ~ 5%(~10% of this luminous)(~10% of this luminous)
NeutrinosNeutrinosmin. 0.1%min. 0.1%max. 6%max. 6%
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Neutrino Mass Limits and Future SensitivityNeutrino Mass Limits and Future Sensitivity
Tritium endpointTritium endpoint2.52.5 eVeV
2020 eVeV
33 eVeV
22 eVeV
11 eVeV
SuperSuper--KamiokandeKamiokande
SN 1987ASN 1987A
0.30.3 eVeV
Mainz/Mainz/TroitskTroitsk
with gravity waveswith gravity waves
with black holewith black hole
0.80.8 eVeV
0.30.3 eVeV
2dF2dF RedshiftRedshift SurveySurvey
SupernovaSupernova NusNusTimeTime--ofof--flightflight
KATRINKATRIN
Cosmic structureCosmic structureSloan Digital Sky SurveySloan Digital Sky Survey
•• Assume 3 massAssume 3 mass eigenstateseigenstates with very small mass differences with very small mass differences as indicated by atmospheric and solar neutrinosas indicated by atmospheric and solar neutrinos
•• The cosmological limit refers toThe cosmological limit refers to mmνν = = ΣΣ mmνν/3/3
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Lecture II: Cosmological NeutrinosLecture II: Cosmological Neutrinos
Neutrino Dark Matter and Neutrino Dark Matter and Cosmic Structure FormationCosmic Structure Formation
Neutrino Chemical Potentials,Neutrino Chemical Potentials,BigBig--BangBang NucleosynthesisNucleosynthesis,,and Flavor Oscillationsand Flavor Oscillations
Neutrino Chemical Potentials,Neutrino Chemical Potentials,BigBig--BangBang NucleosynthesisNucleosynthesis,,and Flavor Oscillationsand Flavor Oscillations
HighestHighest--Energy Cosmic Rays Energy Cosmic Rays and the Cosmic Neutrino Seaand the Cosmic Neutrino Sea
Massive Neutrinos and the Massive Neutrinos and the Cosmic Baryon AsymmetryCosmic Baryon Asymmetry
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
How Many Relic Neutrinos?How Many Relic Neutrinos?
Standard thermal population in one flavorStandard thermal population in one flavor 3113 cm112nn −
γνν ≈= 3113 cm112nn −
γνν ≈=
Additional active Additional active neutrinos beyondneutrinos beyondstandard populationstandard populationof of ννee, , ννµµ, , ννττ
Additional familiesAdditional families Excluded by ZExcluded by Z00 width width ((NNνν = 3) = 3)
Chemical potentials Chemical potentials for for ννee, , ννµµ, , ννττ
PossiblePossible
Sterile Sterile (right(right--handed) handed) statesstates
Populated by Populated by ννLL→→ ννRRtransitionstransitions
Electromagnetic Electromagnetic dipole momentsdipole moments
Excluded by energy loss Excluded by energy loss of globular cluster stars of globular cluster stars
Oscillations/collisionsOscillations/collisions Hot/warm/cold DMHot/warm/cold DMpossiblepossible
RightRight--handed currentshanded currents Excluded by energyExcluded by energyloss of SN 1987A loss of SN 1987A
DiracDirac massmass Not effectiveNot effectivein in eVeV rangerange
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Thermal Neutrino DistributionThermal Neutrino Distribution
FermiFermi--Dirac distributionDirac distribution•• Temperature Temperature TT•• Chemical potential Chemical potential µµ
+µ +µ ParticlesParticles−−µ µ AntiAnti--particles particles
1T
Eexp
1fp+
µ−
=1
TEexp
1fp+
µ−
=
Degeneracy parameterDegeneracy parameterTµ
=ξTµ
=ξ Invariant under cosmic expansionInvariant under cosmic expansion
( )
+ξ
ζ+ξ
ζ+
π
ζ=
ξ+++
ξ−+⌡
⌠
π
π=
ν
νν
...72
13
)2ln(21T23
)T/Eexp(1E
)T/Eexp(1E
24dEn
43
23
323
22
3( )
+ξ
ζ+ξ
ζ+
π
ζ=
ξ+++
ξ−+⌡
⌠
π
π=
ν
νν
...72
13
)2ln(21T23
)T/Eexp(1E
)T/Eexp(1E
24dEn
43
23
323
22
3Number Number densitydensity
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Thermal Neutrino DistributionThermal Neutrino Distribution
FermiFermi--Dirac distributionDirac distribution•• Temperature Temperature TT•• Chemical potential Chemical potential µµ
+µ +µ ParticlesParticles−−µ µ AntiAnti--particles particles
1T
Eexp
1fp+
µ−
=1
TEexp
1fp+
µ−
=
Degeneracy parameterDegeneracy parameterTµ
=ξTµ
=ξ Invariant under cosmic expansionInvariant under cosmic expansion
( )
+ξ
ζ+ξ
ζ+
π
ζ=
ξ+++
ξ−+⌡
⌠
π
π=
ν
νν
...72
13
)2ln(21T23
)T/Eexp(1E
)T/Eexp(1E
24dEn
43
23
323
22
3( )
+ξ
ζ+ξ
ζ+
π
ζ=
ξ+++
ξ−+⌡
⌠
π
π=
ν
νν
...72
13
)2ln(21T23
)T/Eexp(1E
)T/Eexp(1E
24dEn
43
23
323
22
3Number Number densitydensity
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
BBN ConcordanceBBN ConcordanceBurles, Nollett & TurnerBurles, Nollett & Turner
astroastro--ph/9903300ph/9903300
Helium 4Helium 4
DeuteriumDeuterium
LithiumLithium
Cosmic baryon densityCosmic baryon densityimplied by deuteriumimplied by deuteriumΩΩBBhh22 = 0.019 = 0.019 ±± 0.00240.0024
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
BBN Limits on Neutrino FlavorsBBN Limits on Neutrino Flavors
•• At BBN one flavorAt BBN one flavorcontributes aboutcontributes about16% to cosmic16% to cosmicmassmass--energy densityenergy density
•• Extra flavors modifyExtra flavors modifyexpansion parameterexpansion parameteraccordinglyaccordingly
3.43.4 3.23.2 3.03.0
Conservative limitConservative limit|∆|∆NNeffeff|| < 1< 1
Burles, Nollett & Turner, Burles, Nollett & Turner, astroastro--ph/9903300ph/9903300
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
BBN and Neutrino Chemical PotentialsBBN and Neutrino Chemical Potentials
Energy density in one neutrino flavor with Energy density in one neutrino flavor with degeneracy parameter degeneracy parameter ξξ = = ηη/T/T
πξ
+
πξ
+π
=ρ
∆
ννν444 3444 21
effN
4242
715
7301T
1207
πξ
+
πξ
+π
=ρ
∆
ννν444 3444 21
effN
4242
715
7301T
1207
Expansion RateExpansion RateEffectEffect(all flavors)(all flavors)
Beta equilibriumBeta equilibriumeffect foreffect forelectron flavorelectron flavor
−+↔ν+ epn e−+↔ν+ epn e
Helium abundance essentially fixed by Helium abundance essentially fixed by n/p ratio at beta freezen/p ratio at beta freeze--out out
Effect on helium equivalent to Effect on helium equivalent to ∆∆NNeffeff ∼∼ --18 18 ξξννee
( ) epn T/mmepn νξ−−−=
( ) epn T/mmepn νξ−−−=
||∆∆NNeffeff|| < 1< 1 ||ξξννee|| < 0.06 < 0.06
•• ννee beta effect can compensate expansionbeta effect can compensate expansion--rate effect ofrate effect of ννµ,τµ,τ•• No significant BBN limit on neutrino number densityNo significant BBN limit on neutrino number density
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Limits on Radiation DensityLimits on Radiation Density
Allowing foran arbitraryelectron neutrinochemical potential
Allowing forAllowing foran arbitraryan arbitraryelectron neutrinoelectron neutrinochemical potentialchemical potential
Constraints on nuchemical potentials-0.01 < ξνe < 0.25
|ξνµ,τ| < 2.9
Constraints onConstraints on nunuchemical potentialschemical potentials--0.01 0.01 < ξ< ξννee << 0.250.25
|ξ|ξννµ,τµ,τ|| << 2.92.9
Hansen et al.,Hansen et al., astroastro--ph/0105385ph/0105385
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Chemical Potentials and Flavor OscillationsChemical Potentials and Flavor Oscillations
Flavor mixing Flavor mixing (neutrino oscillations)(neutrino oscillations)
Flavor lepton numbersFlavor lepton numbersnot conservednot conserved
Only one commonOnly one common nunuchemical potentialchemical potential
Stringent Stringent ξξννee limit limit applies to all flavors applies to all flavors
||ξξννee,,µ,τµ,τ|| << 0.070.07
Extra neutrino density Extra neutrino density ∆∆NNeffeff << 0.00640.0064
Cosmic neutrino densityCosmic neutrino densityclose to standard valueclose to standard value
nono Solar SMA solutionSolar SMA solution
•• Our knowledge of the cosmicOur knowledge of the cosmic nunudensity depends on the solution ofdensity depends on the solution ofthe solar neutrino problemthe solar neutrino problem
•• KamLANDKamLAND most relevant experimentmost relevant experiment
•• LunardiniLunardini & Smirnov,& Smirnov, hephep--ph/0012056ph/0012056•• DolgovDolgov, Hansen, Pastor,, Hansen, Pastor, PetcovPetcov,, RaffeltRaffelt
&& SemikozSemikoz,, hephep--ph/0201287ph/0201287•• AbazajianAbazajian,, BeacomBeacom & Bell,& Bell,
astroastro--ph/0203442ph/0203442•• Wong,Wong, hephep--ph/0203180 ph/0203180
maybemaybe LOW (depends on LOW (depends on ΘΘ1313))
yesyes Solar LMA solutionSolar LMA solution
Flavor equilibrium before n/pFlavor equilibrium before n/pfreeze outfreeze out ??
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
TwoTwo--Flavor Neutrino OscillationsFlavor Neutrino Oscillations
Evolution of neutrino ensemble described in terms of density matEvolution of neutrino ensemble described in terms of density matricesrices
( )ppp
ep
ep
ep
pp Pf21
ffff
frr ⋅σ+=
=ρ→ µµ
µ( )pp
pep
ep
ep
pp Pf21
ffff
frr ⋅σ+=
=ρ→ µµ
µ
Flavor oscillations in vacuum:Flavor oscillations in vacuum:
p2
pt PBp2
mPrrr
×δ
=∂ p2
pt PBp2
mPrrr
×δ
=∂
withwith
θ
θ=
2cos02sin
Br
θ
θ=
2cos02sin
Br
andand
νν
θθ−θθ
=
νν
µ 21e
cossinsincos
νν
θθ−θθ
=
νν
µ 21e
cossinsincos
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
TwoTwo--Flavor Oscillations in MediaFlavor Oscillations in Media
Neutrinos propagating in a medium suffer refraction (Neutrinos propagating in a medium suffer refraction (WolfensteinWolfenstein 1978)1978)
νν νν
ZZ
ff
νν ff νν
W, ZW, Z
Effect is usually different for different flavorsEffect is usually different for different flavors
Equation of motion in early universe (ignoring neutrino backgrouEquation of motion in early universe (ignoring neutrino background)nd)
pe2W
F2
pt Pzm3
pG28Bp2
mPrrrr
×
ρ−
δ=∂ pe2
W
F2
pt Pzm3
pG28Bp2
mPrrrr
×
ρ−
δ=∂ with with ρρee the ethe e++ee-- energy densityenergy density
Oscillations begin when background medium is sufficiently diluteOscillations begin when background medium is sufficiently diluted tod toavoid large medium effect compared to vacuum mixingavoid large medium effect compared to vacuum mixing
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Flavor Equilibration: LMA SolutionFlavor Equilibration: LMA Solution
DolgovDolgov, Hansen, Pastor, , Hansen, Pastor, PetcovPetcov, , RaffeltRaffelt & & SemikozSemikoz, , hephep--ph/0201287ph/0201287
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Flavor Equilibration: LMA With NonFlavor Equilibration: LMA With Non--Zero Zero ΘΘ1313
DolgovDolgov, Hansen, Pastor, , Hansen, Pastor, PetcovPetcov, , RaffeltRaffelt & & SemikozSemikoz, , hephep--ph/0201287ph/0201287
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Flavor Equilibration: LOW SolutionFlavor Equilibration: LOW Solution
n/p freeze outn/p freeze out
DolgovDolgov, Hansen, Pastor, , Hansen, Pastor, PetcovPetcov, , RaffeltRaffelt & & SemikozSemikoz, , hephep--ph/0201287ph/0201287
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Synchronized Oscillations by SelfSynchronized Oscillations by Self--InteractionsInteractions
Equation of motion in early universe with neutrino backgroundEquation of motion in early universe with neutrino background
with the integrated neutrino polarization vectorswith the integrated neutrino polarization vectors
( ) p3
3
2pd PP ∫
π=
( ) p3
3
2pd PP ∫
π=
( ) p3
3
2pd PP ∫
π=
( ) p3
3
2pd PP ∫
π=
neutrinosneutrinos
antianti--neutrinosneutrinos
andand
( ) pFpe2W
F2
pt G2m3
pG28p2
m PPPPzBP ×−+×
ρ−
δ+=∂ ( ) pFpe2
W
F2
pt G2m3
pG28p2
m PPPPzBP ×−+×
ρ−
δ+=∂
( ) pFpe2W
F2
pt G2m3
pG28p2
m PPPPzBP ×−+×
ρ−
δ−=∂ ( ) pFpe2
W
F2
pt G2m3
pG28p2
m PPPPzBP ×−+×
ρ−
δ−=∂
•• “Magnetic field” caused by neutrinos themselves“Magnetic field” caused by neutrinos themselvesmuch larger than vacuum or medium terms.much larger than vacuum or medium terms.
•• Couples “magnetic moments” to one large dipole Couples “magnetic moments” to one large dipole whichwhich precessesprecesses with a single frequency.with a single frequency.
Pastor,Pastor, RaffeltRaffelt && SemikozSemikoz, PRD 65 (2002) 053011, PRD 65 (2002) 053011
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Synchronized Oscillations by SelfSynchronized Oscillations by Self--InteractionsInteractions
Pastor,Pastor, RaffeltRaffelt && SemikozSemikoz, PRD 65 (2002) 053011, PRD 65 (2002) 053011
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Synchronized Oscillations by SelfSynchronized Oscillations by Self--InteractionsInteractions
Individual modesIndividual modes precessprecess aroundaroundlarge common dipole momentlarge common dipole moment
Pastor,Pastor, RaffeltRaffelt && SemikozSemikoz, PRD 65 (2002) 053011, PRD 65 (2002) 053011
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
ZeroZero--Frequency Synchronized OscillationsFrequency Synchronized Oscillations
( )( )
( )( )∫
∫
−π
+δπ=ω
pp3
3
pp2
3
3
synchPP
2pd
PPp2
m2
pd( )
( )
( )( )∫
∫
−π
+δπ=ω
pp3
3
pp2
3
3
synchPP
2pd
PPp2
m2
pdSynchronized oscillation frequency, Synchronized oscillation frequency, assuming all P vectors start assuming all P vectors start parallel orparallel or antiparallelantiparallel to zto z--axisaxis
p1
2m2
synchδ
=ωp1
2m2
synchδ
=ωOnly neutrinos,Only neutrinos,no antino anti--neutrinosneutrinos
0synch =ω 0synch =ωEqual distribution of neutrinosEqual distribution of neutrinosof one flavor of one flavor and antiand anti--neutrinos of the otherneutrinos of the other
OscillationsOscillationscompletelycompletelysuppressedsuppressed
In a threeIn a three--flavor system, flavor system, oscillations are suppressed oscillations are suppressed (infinitesimally slow) when(infinitesimally slow) when
||ξξ((ννee)| = |)| = |ξξ((ννµµ)| = |)| = |ξξ((ννττ)|)|
Pastor,Pastor, RaffeltRaffelt && SemikozSemikoz, PRD 65 (2002) 053011, PRD 65 (2002) 053011
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Flavor Equilibration: LMA and Flavor Equilibration: LMA and ξξ((ννµµ) = ) = −−ξξ((ννττ) )
DolgovDolgov, Hansen, Pastor, , Hansen, Pastor, PetcovPetcov, , RaffeltRaffelt & & SemikozSemikoz, , hephep--ph/0201287ph/0201287
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
SummarySummary
Confirmation of solar LMAConfirmation of solar LMAsolution bysolution by KamlandKamland
DeDe--facto neutrino flavorfacto neutrino flavorequilibrium before BBNequilibrium before BBN
BBN limit on effectiveBBN limit on effectivenumber ofnumber of nunu flavorsflavors
CosmicCosmic nunu density within 1% of standard valuedensity within 1% of standard value
∑ν
ν =ΩeV94
mh2 ∑
νν =Ω
eV94m
h2
•• Laboratory measurements ofLaboratory measurements of mmνν implyimply ΩΩνν•• StructureStructure--formation limits onformation limits on ΩΩνν directly constraindirectly constrain mmνν
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Lecture II: Cosmological NeutrinosLecture II: Cosmological Neutrinos
Neutrino Dark Matter and Neutrino Dark Matter and Cosmic Structure FormationCosmic Structure Formation
Neutrino Chemical Potentials,Neutrino Chemical Potentials,BigBig--BangBang NucleosynthesisNucleosynthesis,,and Flavor Oscillationsand Flavor Oscillations
HighestHighest--Energy Cosmic Rays Energy Cosmic Rays and the Cosmic Neutrino Seaand the Cosmic Neutrino SeaHighestHighest--Energy Cosmic Rays Energy Cosmic Rays and the Cosmic Neutrino Seaand the Cosmic Neutrino Sea
Massive Neutrinos and the Massive Neutrinos and the Cosmic Baryon AsymmetryCosmic Baryon Asymmetry
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Global Cosmic Ray SpectrumGlobal Cosmic Ray Spectrum
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
GreisenGreisen--ZatsepinZatsepin--KuzminKuzmin (GZK) Cutoff(GZK) Cutoff
PRL 16 (1966) 748PRL 16 (1966) 748PRL 16 (1966) 748
One event (1962) with 1020 eV
One event (1962) One event (1962) with 10with 102020 eVeV
p + γ → ∆+ → p + π0→p + p + γγ → ∆∆++ →→ p + p + ππ00
JETP Lett. 4 (1966) 78JETP JETP LettLett. . 4 (1966) 784 (1966) 78
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Spectrum of HighestSpectrum of Highest--Energy AGASA EventsEnergy AGASA Events
astroastro--ph/0008102ph/0008102
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
ZZ--Bursts and HighestBursts and Highest--Energy Cosmic RaysEnergy Cosmic Rays
NeutrinosNeutrinosEEνν ~ 10~ 102121 -- 10102222 eVeVfrom unknown sourcesfrom unknown sources
Cosmic relic Cosmic relic neutrinosneutrinosmmνν ~ 1 ~ 1 eVeV
ResonantResonantZZ--BosonBoson
ProductionProduction
Neutrino energyNeutrino energyon resonanceon resonance
eV
212Z
meV102.4
m2M
E ×==
νν
eV
212Z
meV102.4
m2M
E ×==
νν
DecayDecay(Z(Z--Burst)Burst)
On averageOn average2 Nucleons2 Nucleons10 10 ππ00 →→ 20 20 γγ17 17 ππ±± →→ ee±± νν νν
Measured cosmic raysMeasured cosmic rays
For example: For example: •• WeilerWeiler
hephep--ph/9710431ph/9710431•• FargionFargion et al.et al.
hephep--ph/0112014ph/0112014•• Fodor, Katz, Fodor, Katz, RingwaldRingwald
hephep--ph/0203198ph/0203198
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Fitting the Cosmic Ray Spectrum with ZFitting the Cosmic Ray Spectrum with Z--BurstsBursts
Cosmic ray spectrum near cutoff can be fit for Cosmic ray spectrum near cutoff can be fit for a wide range of allowed neutrino massesa wide range of allowed neutrino masses
Main problemsMain problems•• Huge source flux of Huge source flux of
EHE neutrinosEHE neutrinosrequiredrequired
•• No plausible sourcesNo plausible sourcesknownknown
•• Accompanying Accompanying photons must bephotons must beperfectly obscuredperfectly obscured
KalashevKalashev et al. et al. hephep--ph/0112351ph/0112351
Fodor, Katz & Fodor, Katz & RingwaldRingwald, , hephep--ph/0203198ph/0203198
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Discovery Potential for Required Neutrino FluxesDiscovery Potential for Required Neutrino Fluxes
Discovering an EHE neutrino fluxat this level might allow one tosee evidence for cosmic relicneutrinos
Discovering an EHE neutrino fluxDiscovering an EHE neutrino fluxat this level might allow one toat this level might allow one tosee evidence for cosmic relicsee evidence for cosmic relicneutrinosneutrinos
Fodor, Katz & Ringwald, hep-ph/0203198Fodor, Katz & Fodor, Katz & RingwaldRingwald, , hephep--ph/0203198ph/0203198
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Lecture II: Cosmological NeutrinosLecture II: Cosmological Neutrinos
Neutrino Dark Matter and Neutrino Dark Matter and Cosmic Structure FormationCosmic Structure Formation
Neutrino Chemical Potentials,Neutrino Chemical Potentials,BigBig--BangBang NucleosynthesisNucleosynthesis,,and Flavor Oscillationsand Flavor Oscillations
HighestHighest--Energy Cosmic Rays Energy Cosmic Rays and the Cosmic Neutrino Seaand the Cosmic Neutrino Sea
Massive Neutrinos and the Massive Neutrinos and the Cosmic Baryon AsymmetryCosmic Baryon AsymmetryMassive Neutrinos and the Massive Neutrinos and the Cosmic Baryon AsymmetryCosmic Baryon Asymmetry
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
BaryogenesisBaryogenesis in the Early Universein the Early Universe
SakharovSakharov conditions for creating the conditions for creating the BBaryon aryon AAsymmetry of the symmetry of the UUniverse (niverse (BAUBAU))•• C and CP violationC and CP violation•• Baryon number violationBaryon number violation•• Deviation from thermal equilibriumDeviation from thermal equilibrium
ParticleParticle--physics standard modelphysics standard model•• Violates B and L byViolates B and L by electroweakelectroweak instantoninstanton effects effects •• Conserves B Conserves B –– LL
In cosmological evolutionIn cosmological evolution•• PrePre--existing B+L erased at EW phase transitionexisting B+L erased at EW phase transition•• Creation of BAU at phase transition not possible, Creation of BAU at phase transition not possible, except for special parameters in SUSY modelsexcept for special parameters in SUSY models
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
LeptogenesisLeptogenesis by by MajoranaMajorana Neutrino DecaysNeutrino Decays
Another classic paperAnother classic paperAnother classic paper
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
SeeSee--Saw Model for Neutrino MassesSaw Model for Neutrino Masses
NeutrinosNeutrinosNeutrinosCharged LeptonsCharged LeptonsCharged Leptons
DiracDirac massesmassesfrom couplingfrom couplingto standardto standardHiggs field Higgs field φφ
HeavyHeavyMajoranaMajoranamassesmasses MMjj
Lagrangian forparticle massesLagrangianLagrangian forforparticle massesparticle masses .c.hMNN
21NgegL R
cRRLRLmass +−φ−φ−= νll l .c.hMNN
21NgegL R
cRRLRLmass +−φ−φ−= νll l
LightLight MajoranaMajorana massmass
( )
ν
φ
ν
ν
RL
22
RL NM0
0M
g
N( )
ν
φ
ν
ν
RL
22
RL NM0
0M
g
N( )
ν
φ
φν
ν
ν
RL
RL NMgg0
N( )
ν
φ
φν
ν
ν
RL
RL NMgg0
N DiagonalizeDiagonalizeDiagonalize
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Leptogenesis by OutLeptogenesis by Out--ofof--Equilibrium DecayEquilibrium Decay
Equilibrium abundance ofheavy Majorana neutrinosEquilibrium abundance ofEquilibrium abundance ofheavyheavy MajoranaMajorana neutrinosneutrinos
Real non-equilibrium abundancedetermined by decay rateReal nonReal non--equilibrium abundanceequilibrium abundancedetermined by decay ratedetermined by decay rate
Lepton-number abundancecreated by CP-violating decaysLeptonLepton--number abundancenumber abundancecreated by CPcreated by CP--violating decaysviolating decays
CP-violating decays byinterference of tree-levelwith one-loop diagram
CPCP--violating decays byviolating decays byinterference of treeinterference of tree--levellevelwith onewith one--loop diagramloop diagram
πν=Γ 8M2
Decay g πν=Γ 8M2
Decay g
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Connection to Neutrino MassConnection to Neutrino Mass
πν=Γ 8M2
Decay g πν=Γ 8M2
Decay g Decay rate of heavy MajorananeutrinoDecay rate of heavyDecay rate of heavy MajoranaMajorananeutrinoneutrino
Pl
2mT
effgH ≈Pl
2mT
effgH ≈ Cosmic expansion rateCosmic expansion rateCosmic expansion rate
MTDecay H =<Γ MTDecay H =<Γ Requirement for strong deviationfrom equilibrium ...Requirement for strong deviationRequirement for strong deviationfrom equilibrium ...from equilibrium ...
Pl
2
mM
eff2 g
8Mg <πν Pl
2
mM
eff2 g
8Mg <πν
Pleff
mg82
Mg πν <
Pleff
mg82
Mg πν <
eV10~M
gm 32m
g822
Pleff −πν
ν φ<φ
= eV10~M
gm 32m
g822
Pleff −πν
ν φ<φ
=... translates into a limit on the
observable neutrino mass... translates into a limit on the... translates into a limit on the
observable neutrino massobservable neutrino mass
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
LeptogenesisLeptogenesis by by MajoranaMajorana Neutrino DecaysNeutrino Decays
In see-saw models of neutrino masses, right-handed heavy Majorana neutrinos provide source for L-violationIn seeIn see--saw models of neutrino masses, rightsaw models of neutrino masses, right--handed handed heavy heavy MajoranaMajorana neutrinos provide source for Lneutrinos provide source for L--violationviolation
Cosmological evolution:• B = L = 0 early on• Thermal freeze-out of heavy Majorana neutrinos• Out-of-equilibrium CP-violating decay creates net L• Shift L excess into B by sphaleron effects
Cosmological evolution:Cosmological evolution:•• B = L = 0 early onB = L = 0 early on•• Thermal freezeThermal freeze--out of heavy out of heavy MajoranaMajorana neutrinosneutrinos•• OutOut--ofof--equilibrium CPequilibrium CP--violating decay creates net Lviolating decay creates net L•• Shift L excess into B byShift L excess into B by sphaleronsphaleron effectseffects
Sufficient deviation from equilibrium distribution of heavy Majorana neutrinos at freeze-out
Sufficient deviation from Sufficient deviation from equilibrium distribution of equilibrium distribution of heavy heavy MajoranaMajorana neutrinos neutrinos at freezeat freeze--outout
LimitsonYukawacouplings
LimitsLimitsononYukawaYukawacouplingscouplings
Limitson lightneutrinomasses
LimitsLimitson on lightlightneutrinoneutrinomassesmasses
Consistent with hierarchical masses below 0.1 eVConsistent with hierarchical masses below 0.1 Consistent with hierarchical masses below 0.1 eVeV
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
LeptogenesisLeptogenesis –– A Popular Research TopicA Popular Research TopicLangackerLangacker, , Peccei Peccei & & YanagidaYanagidaMod. Phys. Mod. Phys. LettLett. A 1 (1986) 541. A 1 (1986) 541
Campbell, Davidson & OliveCampbell, Davidson & OliveNPB 399 (1993) 111NPB 399 (1993) 111
Fukugita Fukugita & & YanagidaYanagidaPLB 174 (1986) 45PLB 174 (1986) 45
GherghettaGherghetta & & JungmannJungmannPRD 48 (1993) 1546PRD 48 (1993) 1546
MuryamaMuryama & & YanagidaYanagidaPLB 322 (1994) 349PLB 322 (1994) 349
Dine, Randall & ThomasDine, Randall & ThomasNPB 458 (1996) 291NPB 458 (1996) 291
WorahWorahPRD 53 (1996) 3902PRD 53 (1996) 3902
Buchmüller Buchmüller & & PlümacherPlümacherPLB 389 (1996) 73 PLB 389 (1996) 73
Ma & Ma & SarkarSarkarPRL 80 (1998) 5716PRL 80 (1998) 5716
JeannerotJeannerotPRLPRL 7777 (1996)(1996) 32923292
LazaridesLazarides, Schaefer & , Schaefer & ShafiShafiPRD 56 (1997) 1324PRD 56 (1997) 1324
PlümacherPlümacherNPB 530 (1998) 207NPB 530 (1998) 207
LazaridesLazarides & & ShafiShafiPRD 58 (1998) 071702PRD 58 (1998) 071702
FlanzFlanz & & PaschosPaschosPRD 58 (1998) 113009PRD 58 (1998) 113009
Ellis, Lola & Ellis, Lola & NanopoulosNanopoulosPLB 452 (1999) 87PLB 452 (1999) 87
Berger & Berger & BrahmachariBrahmachariPRD 60 (1999) 073009PRD 60 (1999) 073009
CarlierCarlier, Frére & Ling, Frére & LingPRD 60 (1999) 096003PRD 60 (1999) 096003
AkhmedovAkhmedov, , RubakovRubakov & Smirnov& SmirnovPRL 81 (1998) 1562PRL 81 (1998) 1562
GiudiceGiudice, , PelosoPeloso, , RiottoRiotto & & TkachevTkachevJHEP 9908 (1999) 014JHEP 9908 (1999) 014
Frére, Ling, Frére, Ling, TytgatTytgat & v.& v.ElewyckElewyckPRD 60 (1999) 016005PRD 60 (1999) 016005
BarbieriBarbieri, , CreminelliCreminelli, , StrumiaStrumia & & TetradisTetradisNPB 575 (2000) 61NPB 575 (2000) 61
BergerBergerPRD 62 (2000) 013007PRD 62 (2000) 013007
HambyeHambye, Ma & , Ma & SarkarSarkarPRD 62 (2000) 015010PRD 62 (2000) 015010
GoldbergGoldbergPLBPLB 474474 (2000)(2000) 389389
AsakaAsaka, , HamaguchiHamaguchi, Kawasaki & , Kawasaki & YanagidaYanagidaPRD 61 (2000) 083512PRD 61 (2000) 083512
Dick, Lindner, Dick, Lindner, RatzRatz & Wright& WrightPRL 84 (2000) 4039PRL 84 (2000) 4039
LalakulichLalakulich, , PaschosPaschos & & FlanzFlanzPRD 62 (2000) 053006PRD 62 (2000) 053006
RangarajanRangarajan & & MishraMishraPRDPRD 6161 (2000)(2000) 043509043509
ManganoMangano & & MieleMielePRDPRD 6262 (2000)(2000) 063514063514
BasteroBastero--Gil & King Gil & King PRD 63 (2001) 123509PRD 63 (2001) 123509
Joshipura, Paschos & RodejohannJoshipura, Paschos & RodejohannNPB 611 (2001) 227NPB 611 (2001) 227
Falcone & TramontanoFalcone & TramontanoPRD PRD 6363 (2001) 073007(2001) 073007
HambyeHambye, Ma & , Ma & SarkarSarkarNPB 602 (2001) 23NPB 602 (2001) 23
Hirsch & KingHirsch & KingPRD 64 (2001) 113005PRD 64 (2001) 113005
Branco, Morozumi, Nobre & RebeloBranco, Morozumi, Nobre & RebeloNPB 617 (2001) 475NPB 617 (2001) 475 AND MANY MORE ...AND MANY MORE ...
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrinos and Cosmology, Beijing, China (20-25 August 2002)
Conclusions of Lecture IIConclusions of Lecture II
LargeLarge--scale galaxyscale galaxy redshiftredshift surveyssurveys•• Best limit ofBest limit of mmνν << 0.80.8 eVeV,,•• Future sensitivity ~ 0.3Future sensitivity ~ 0.3 eVeV
If solar LMA solution applies,If solar LMA solution applies,cosmic neutrino number densitycosmic neutrino number densityprecisely determined by BBNprecisely determined by BBN
If highestIf highest--E cosmicE cosmic--ray neutrinos are found,ray neutrinos are found,ZZ--bursts provide handle onbursts provide handle on mmνν
MajoranaMajorana neutrino masses in the favored neutrino masses in the favored range suggest arange suggest a leptogenesisleptogenesis scenario scenario for generating cosmic baryon asymmetryfor generating cosmic baryon asymmetry