Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002 Massive Neutrinos Georg Raffelt Max-Planck-Institut für Physik, München, Germany From Here to Infinity: Extending Frontiers in Cosmology A Weekend Symposium to Celebrate the Sixtieth Birthday of Joseph Silk Oxford, England, December 13-15, 2002 News from the Ghost Particles
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Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Massive NeutrinosMassive Neutrinos
Georg RaffeltMax-Planck-Institut für Physik, München,
Germany
Georg RaffeltMax-Planck-Institut für Physik, München,
Germany
From Here to Infinity: Extending Frontiers in Cosmology
A Weekend Symposium to Celebrate the Sixtieth Birthday of Joseph Silk Oxford, England, December 13-15, 2002
From Here to Infinity: Extending Frontiers in Cosmology
A Weekend Symposium to Celebrate the Sixtieth Birthday of Joseph Silk Oxford, England, December 13-15, 2002
News from the Ghost ParticlesNews from the Ghost Particles
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
22 eV/m 22 eV/m LMALMA 0.2-2 or 6.50.2-2 or 6.5310)45.1( 410)22.0(
Mutually inconsistent, even with a sterile neutrinoMutually inconsistent, even with a sterile neutrinoEvidenceEvidence forfor physicsphysics beyondbeyond flavorflavor oscillations (CPT violation ...) ?oscillations (CPT violation ...) ?ImplicationImplication
A MiniBooNEA MiniBooNEconfirmation of LSND wouldconfirmation of LSND would
be another revolutionbe another revolution ..Too good to be trueToo good to be true ??
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Japanese nuclear reactorsJapanese nuclear reactors60 GW (20% world capacity)60 GW (20% world capacity)
• Witout OscillationsWitout Oscillations 2 Neutrino captures / day2 Neutrino captures / day• Data taking sinceData taking since 22 January 200222 January 2002
First Kamland results earlier this weekFirst Kamland results earlier this weekat “Texas in Tuscany” and hep-ex/0212021at “Texas in Tuscany” and hep-ex/0212021
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
• How large is How large is 1313 ??• CP-violating phaseCP-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 ??
Tasks and Open QuestionsTasks and Open Questions
• Precision for Precision for 12 12 andand 2323
((12 12 < 45º and < 45º and 23 23 45º 45º ?) ?)
• How large is How large is 1313 ??• CP-violating phaseCP-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 ??
CosmologyCosmologyCosmologyCosmology
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Scaled-up spectrometer (KATRIN) may reach 0.3 eVScaled-up spectrometer (KATRIN) may reach 0.3 eVCurrently in preparation - Results in > 5 yearsCurrently in preparation - Results in > 5 years
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Cosmological Limit on Neutrino MassesCosmological Limit on Neutrino Masses
A classic paper:A classic paper: Gershtein & ZeldovichGershtein & Zeldovich JETP Lett. 4 (1966) 120JETP Lett. 4 (1966) 120
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Neutrino Mass Limit from 2dF Galaxy SurveyNeutrino Mass Limit from 2dF Galaxy Survey
Elgaroy et al., Elgaroy et al., astro-ph/0204152astro-ph/0204152
= = 0.010.01
= = 00
Similar limits basedSimilar limits basedon the 2dF survey on the 2dF survey • HannestadHannestad astro-ph/0205223astro-ph/0205223• Lewis & BridleLewis & Bridle astro-ph/0205436astro-ph/0205436
= = 0.050.05
mm < 2.2 eV < 2.2 eV
at 95% CLat 95% CL(statistical)(statistical)
Depends on priors forDepends on priors forother parametersother parameters
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
PLANCK Sensitivity to Neutrino MassPLANCK Sensitivity to Neutrino Mass
Maximum Maximum temperature multipoletemperature multipole that can be that can bemeasured to cosmic-variance precisionmeasured to cosmic-variance precision
• At BBN one flavorAt BBN one flavor contributes aboutcontributes about 16% to cosmic16% to cosmic mass-energy mass-energy densitydensity• Extra flavors Extra flavors modifymodify expansion expansion parameterparameter accordinglyaccordingly
Conservative limitConservative limit
NNeffeff < 1 < 1
3.43.4 3.23.2 3.03.0
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
BBN and Neutrino Chemical PotentialsBBN and Neutrino Chemical Potentials
• e e beta effect can compensate expansion-rate effect of beta effect can compensate expansion-rate effect of • No significant BBN limit on neutrino number densityNo significant BBN limit on neutrino number density
Energy density in one neutrino flavor with Energy density in one neutrino flavor with degeneracy parameter degeneracy parameter = = /T/T
effN
424
2
715
730
1T1207
effN
424
2
715
730
1T1207
Expansion RateExpansion Rate
EffectEffect
(all flavors)(all flavors)
Beta equilibriumBeta equilibrium
effect foreffect for
electron flavorelectron flavor epn e epn e
Helium abundance essentially fixed by Helium abundance essentially fixed by n/p ratio at beta freeze-out n/p ratio at beta freeze-out
Effect on helium equivalent to Effect on helium equivalent to NNeffeff -18 -18 ee
epn T/mme
pn
epn T/mme
pn
NNeffeff < 1 < 1 ee < 0.06 < 0.06
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Chemical Potentials and Flavor OscillationsChemical Potentials and Flavor Oscillations
• Our knowledge of the cosmic nuOur knowledge of the cosmic nu density depends on the solution ofdensity depends on the solution of the solar neutrino problemthe solar neutrino problem• KamLAND most relevant experimentKamLAND most relevant experiment
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Baryogenesis in the Early UniverseBaryogenesis in the Early Universe
Sakharov conditions for creating the Sakharov 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
Particle-physics standard modelParticle-physics standard model• Violates C and CPViolates C and CP• Violates B and L by EW instanton effectsViolates B and L by EW instanton effects (B – L conserved)(B – L conserved)
• However, electroweak baryogenesis not However, electroweak baryogenesis not quantitativelyquantitatively possible within particle-physics standard modelpossible within particle-physics standard model• Works in SUSY models for small range of Works in SUSY models for small range of parametersparameters
Andrei SakharovAndrei Sakharov1921 - 19891921 - 1989
A.Riotto & M.Trodden: A.Riotto & M.Trodden: Recent progress in baryogenesis Recent progress in baryogenesis Ann. Rev. Nucl. Part. Sci. 49 (1999) 35Ann. Rev. Nucl. Part. Sci. 49 (1999) 35
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Leptogenesis by Majorana Neutrino DecaysLeptogenesis by Majorana Neutrino Decays
A classic paperA classic paper
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
See-Saw Model for Neutrino MassesSee-Saw Model for Neutrino Masses
NeutrinosNeutrinosCharged LeptonsCharged Leptons
Lagrangian for Lagrangian for particle massesparticle masses
cRRLmas Rs L Rg e g
1NL h.c.MNN
2 cRRLmas Rs L Rg e g
1NL h.c.MNN
2
Dirac massesDirac masses from couplingfrom coupling to standardto standard Higgs field Higgs field
HeavyHeavy Majorana Majorana masses masses
MMjj > 10 > 101010 GeV GeV
LL R
R
0 gN
Ng M
LL R
R
0 gN
Ng M
DiagonalizeDiagonalize DiagonalizeDiagonalize
2 2
LL R
R
gM
0N
N0 M
2 2
LL R
R
gM
0N
N0 M
Light Majorana massLight Majorana mass
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
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
Leptogenesis by Out-of-Equilibrium DecayLeptogenesis by Out-of-Equilibrium Decay
CP-violating decays byCP-violating decays by interference of tree-levelinterference of tree-level with one-loop diagramwith one-loop diagram
Real abundanceReal abundancedetermined bydetermined bydecay ratedecay rate
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
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 decay of right-handed heavy Majorana neutrinos providesdecay of right-handed heavy Majorana neutrinos provides source for CP- and L-violationsource for CP- and L-violation
Cosmological evolution:Cosmological 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 onLimits on masses masses ofof ordinaryordinary neutrinosneutrinos
Requires Majorana neutrino masses below 0.2 eVRequires Majorana neutrino masses below 0.2 eVBuchmüller, Di Bari & Plümacher, PLB 547 (2002) 128 [hep-ph/0209301]Buchmüller, Di Bari & Plümacher, PLB 547 (2002) 128 [hep-ph/0209301]
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Leptogenesis – A Popular Research TopicLeptogenesis – A Popular Research Topic Langacker, Peccei & YanagidaLangacker, Peccei & Yanagida Mod. Phys. Lett. A 1 (1986) 541Mod. Phys. Lett. A 1 (1986) 541
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 From Here to Infinity, Oxford, England, 13-15 December 2002
Neutrinoless Neutrinoless Decay Decay
76Ge76Ge
76Se76Se
76As76As
O+O+
2–2–
2+2+
O+O+
Some nuclei decay onlySome nuclei decay onlyby the by the mode, e.g. mode, e.g.Some nuclei decay onlySome nuclei decay onlyby the by the mode, e.g. mode, e.g.
Half life ~ 10Half life ~ 102121 yr yrHalf life ~ 10Half life ~ 102121 yr yr
N 2ee i ei i
i 1m U m
N 2ee i ei i
i 1m U m
MeasureMeasure
ddquantityquantity
eem 0.35eVeem 0.35eVBest Best limitlimitfrom from 7676GeGe
00mode, enabledmode, enabledby Majorana massby Majorana mass Standard 2Standard 2modemode
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Summary of Current Neutrinoless Summary of Current Neutrinoless Decay Decay LimitsLimits
O.C
rem
on
esi
at
Neu
trin
o 2
00
2O
.Cre
mon
esi
at
Neu
trin
o 2
00
2
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Summary of Future Summary of Future Decay Projects Decay ProjectsO
.Cre
mon
esi
at
Neu
trin
o 2
00
2O
.Cre
mon
esi
at
Neu
trin
o 2
00
2
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 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)
NeutrinosNeutrinos min. 0.1%min. 0.1% max. 6%max. 6%