massive neutrinos
Post on 01-Feb-2016
58 Views
Preview:
DESCRIPTION
TRANSCRIPT
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
AtmosphericAtmospheric SolarSolar LSNDLSNDSystemSystem
Status of Evidence for Neutrino OscillationsStatus of Evidence for Neutrino Oscillations
StatusStatus EstablishedEstablished EstablishedEstablished UnconfirmedUnconfirmed
TestTest Long BaselineLong Baseline KamLAND 12/2002KamLAND 12/2002 MiniBooNE 2004 ?MiniBooNE 2004 ?
Three mass eigenstates withThree mass eigenstates withmm11 << m << m22 << m << m33 ~ 50 meV (hierarchical) ~ 50 meV (hierarchical)mm11 ~ m ~ m22 ~ m ~ m33 >> 50 meV (degenerate) >> 50 meV (degenerate)
SimplestSimplestinterpre-interpre-tationtation
Experimental orExperimental orStatisticalStatistical
FlukeFluke
e e e eChannelChannel
2sin2 2sin2 0.90.911 0.20.20.60.6 0.0010.0010.030.03
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
Kamland Reactor Neutrino Experiment (Japan)Kamland Reactor Neutrino Experiment (Japan)
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
Three-Flavor Neutrino Parameters (Ignoring Three-Flavor Neutrino Parameters (Ignoring LSND)LSND)
1
2
3
e 13 13 12 12
23 23 12 12
23 23 13 13
i
i
1 C S C S
C S 1 S C
S C 1S C
e
e
1
2
3
e 13 13 12 12
23 23 12 12
23 23 13 13
i
i
1 C S C S
C S 1 S C
S C 1S C
e
e
CP-violating phaseCP-violating phase12 12C cos etc., 12 12C cos etc.,
AtmosphericAtmospheric Chooz LimitChooz Limit SolarSolar
2 2m meV 2 2m meV
SolarSolar2424 --240240
AtmosphericAtmospheric14001400 --60006000
33 ranges rangeshep-ph/0211054hep-ph/0211054
2332 60 2332 60 1227 41 1227 41 13 14 13 14
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
((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 ??
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
Tritium Endpoint SpectrumTritium Endpoint Spectrum
Electron spectrum N(E)Electron spectrum N(E)
EE
mm
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
Mainz Experiment, PLB 460 (1999) 219Mainz Experiment, PLB 460 (1999) 219
m < 2.8 eV (95% CL)m < 2.8 eV (95% CL)
Troitsk Experiment, ibid. 227Troitsk Experiment, ibid. 227
m < 2.5 eV (95% CL)m < 2.5 eV (95% CL)
TheseTheseexperimentsexperimentshave reachedhave reached2.2 eV2.2 eV(Neutrino(Neutrino 2002)2002)
Tritium Beta DecayTritium Beta Decay
Endpoint energy 18.6 keVEndpoint energy 18.6 keVe
33 eHeH e
33 eHeH
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
Maxim
um
M
axim
um
pola
riza
tion
mu
ltip
ole
pola
riza
tion
mu
ltip
ole
th
at
can
be
th
at
can
be
measu
red
to c
osm
ic-v
ari
an
ce p
reci
sion
measu
red
to c
osm
ic-v
ari
an
ce p
reci
sion
0.07 0.07 eVeV
0.07 0.07 eVeV
0.13 0.13 eVeV
0.13 0.13 eVeV
0.25 0.25 eVeV
0.25 0.25 eVeV
Steen HannestadSteen Hannestadastro-ph/0211106astro-ph/0211106
11 sensitivity to sensitivity to mm
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
1010-2-2 1010-1-1 11 10 10 eVeV
3m 3
m
1010-3-3 1010-2-2 1010-1-1 11 Assuming h = 0.75Assuming h = 0.75
Mass-Energy-Inventory of the UniverseMass-Energy-Inventory of the Universe
luminousluminous TotalTotalBaryonsBaryons
Dark MatterDark Matter
Tritium Tritium Mainz/TroitskMainz/Troitsk
KATRIN, SDSS (Future)KATRIN, SDSS (Future)
PLANCK+SDSS (“Optimistic” future)PLANCK+SDSS (“Optimistic” future)
Super-KSuper-K NeutrinosNeutrinosNeutrinosNeutrinosSuper-KSuper-K 2dF Galaxy Survey2dF Galaxy Survey
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
Additional active Additional active neutrinos beyondneutrinos beyondstandard populationstandard population
of of ee, , , ,
How Many Relic Neutrinos?How Many Relic Neutrinos?
Sterile Sterile (right-handed) (right-handed) statesstates
Populated by Populated by LL R R
transitionstransitions
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
Right-handed currentsRight-handed currents Excluded by energyExcluded by energyloss of SN 1987A loss of SN 1987A
Dirac massDirac mass Not effectiveNot effectivein eV rangein eV range
Additional familiesAdditional familiesExcluded by ZExcluded by Z00 width width
(N(N = 3) = 3)
Chemical potentials Chemical potentials
for for ee, , , , PossiblePossible
Standard thermal population in one flavorStandard thermal population in one flavor 3113 cm112nn
3113 cm112nn
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany From Here to Infinity, Oxford, England, 13-15 December 2002
BBN Limits on Neutrino FlavorsBBN Limits on Neutrino Flavors
Burles, Nollett & Turner, Burles, Nollett & Turner, astro-ph/9903300astro-ph/9903300
• 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
• Lunardini & Smirnov, hep-ph/0012056 Lunardini & Smirnov, hep-ph/0012056 • Dolgov, Hansen, Pastor, Petcov, RaffeltDolgov, Hansen, Pastor, Petcov, Raffelt & Semikoz, hep-ph/0201287& Semikoz, hep-ph/0201287• Abazajian, Beacom & Bell,Abazajian, Beacom & Bell, astro-ph/0203442astro-ph/0203442• Wong, hep-ph/0203180 Wong, hep-ph/0203180
nono SMA or VACSMA or VAC
maybemaybe LOW (depends on LOW (depends on 1313))
yesyes Solar LMA solutionSolar LMA solution
Flavor equilibrium before n/pFlavor equilibrium before n/pfreeze outfreeze out ??
Stringent Stringent ee limit limit
applies to all flavors applies to all flavors
||ee|| 0.07 0.07
Cosmic neutrino densityCosmic neutrino densityclose to standard valueclose to standard value
Extra neutrino density Extra neutrino density NNeffeff 0.0064 0.0064
Only one common nu Only one common nu chemical potentialchemical potential
Flavor mixing Flavor mixing (neutrino oscillations)(neutrino oscillations)
Flavor lepton numbersFlavor lepton numbersnot conservednot conserved
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
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
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
8M2
Decay g 8M2
Decay g
EquilibriumEquilibriumabundance ofabundance ofheavy Majoranaheavy Majorananeutrinosneutrinos
Real abundanceReal abundancedetermined bydetermined bydecay ratedecay rate
CreatedCreatedlepton-numberlepton-numberabundanceabundance
EquilibriumEquilibriumabundance ofabundance ofheavy Majoranaheavy Majorananeutrinosneutrinos
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 Limits onon YukawaYukawa couplingcouplingss
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
Campbell, Davidson & OliveCampbell, Davidson & Olive NPB 399 (1993) 111NPB 399 (1993) 111
Fukugita Fukugita & & YanagidaYanagida PLB 174 (1986) 45PLB 174 (1986) 45
Gherghetta & JungmannGherghetta & JungmannPRD 48 (1993) 1546PRD 48 (1993) 1546
Muryama & YanagidaMuryama & YanagidaPLB 322 (1994) 349PLB 322 (1994) 349
Dine, Randall & ThomasDine, Randall & Thomas NPB 458 (1996) 291NPB 458 (1996) 291
WorahWorahPRD 53 (1996) 3902PRD 53 (1996) 3902
Buchmüller & PlümacherBuchmüller & Plümacher PLB 389 (1996) 73 PLB 389 (1996) 73
Ma & SarkarMa & SarkarPRL 80 (1998) 5716PRL 80 (1998) 5716
JeannerotJeannerotPRLPRL 7777 (1996)(1996) 32923292
Lazarides, Schaefer & ShafiLazarides, Schaefer & Shafi PRD 56 (1997) 1324PRD 56 (1997) 1324
PlümacherPlümacherNPB 530 (1998) 207NPB 530 (1998) 207
Lazarides & ShafiLazarides & ShafiPRD 58 (1998) 071702PRD 58 (1998) 071702
Flanz & PaschosFlanz & PaschosPRD 58 (1998) 113009PRD 58 (1998) 113009
Ellis, Lola & NanopoulosEllis, Lola & NanopoulosPLB 452 (1999) 87PLB 452 (1999) 87
Berger & BrahmachariBerger & BrahmachariPRD 60 (1999) 073009PRD 60 (1999) 073009
Carlier, Frére & LingCarlier, Frére & LingPRD 60 (1999) 096003PRD 60 (1999) 096003
Akhmedov, Rubakov & SmirnovAkhmedov, Rubakov & SmirnovPRL 81 (1998) 1562PRL 81 (1998) 1562
Giudice, Peloso, Riotto & TkachevGiudice, Peloso, Riotto & TkachevJHEP 9908 (1999) 014JHEP 9908 (1999) 014
Frére, Ling, Tytgat & v.ElewyckFrére, Ling, Tytgat & v.ElewyckPRD 60 (1999) 016005PRD 60 (1999) 016005
Barbieri, Creminelli, Strumia & TetradisBarbieri, Creminelli, Strumia & TetradisNPB 575 (2000) 61NPB 575 (2000) 61
BergerBergerPRD 62 (2000) 013007PRD 62 (2000) 013007
Hambye, Ma & SarkarHambye, Ma & SarkarPRD 62 (2000) 015010PRD 62 (2000) 015010
GoldbergGoldbergPLBPLB 474474 (2000)(2000) 389389
Asaka, Hamaguchi, Kawasaki & YanagidaAsaka, Hamaguchi, Kawasaki & YanagidaPRD 61 (2000) 083512PRD 61 (2000) 083512
Dick, Lindner, Ratz & WrightDick, Lindner, Ratz & WrightPRL 84 (2000) 4039PRL 84 (2000) 4039
Lalakulich, Paschos & FlanzLalakulich, Paschos & FlanzPRD 62 (2000) 053006PRD 62 (2000) 053006
Rangarajan & MishraRangarajan & MishraPRDPRD 6161 (2000)(2000) 043509043509
Mangano & MieleMangano & MielePRDPRD 6262 (2000)(2000) 063514063514
Bastero-Gil & King Bastero-Gil & King PRD 63 (2001) 123509PRD 63 (2001) 123509
Joshipura, Paschos & RodejohannJoshipura, Paschos & Rodejohann NPB 611 (2001) 227NPB 611 (2001) 227
Falcone & TramontanoFalcone & Tramontano PRD PRD 6363 (2001) 073007(2001) 073007
Hambye, Ma & SarkarHambye, Ma & Sarkar NPB 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 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%
top related