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18 Feb. 2005, E.J.Chun, KIAS18 Feb. 2005, E.J.Chun, KIAS Workshop for Underground Experiment and AstrWorkshop for Underground Experiment and Astroparticle Physics, Muju, 2005. 2. 16-19oparticle Physics, Muju, 2005. 2. 16-19
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Neutrinoless Double BetNeutrinoless Double Beta Decaya Decay
Eung Jin ChunEung Jin ChunKorea Institute for Advanced StudyKorea Institute for Advanced Study
APS neutrino study: physics/0411216APS neutrino study: physics/0411216 hep-ph/0412300hep-ph/0412300 Bilenky, et.al., hep-ph/0402250Bilenky, et.al., hep-ph/0402250
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18 Feb. 2005, E.J.Chun, KIAS Workshop for Underground Experiment and Astroparticle Physics, Muju, 2005. 2. 16-19
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Key questions by theoristsKey questions by theorists APS neutrino study: physics/0411216APS neutrino study: physics/0411216
►Are neutrinos their own anti-particles?Are neutrinos their own anti-particles?►What is the pattern of neutrino masses?What is the pattern of neutrino masses?► Is there CP violation in the leptonic sector? Is there CP violation in the leptonic sector?
-- -- Possibly the origin of the matter-antimatter asymmetry of the universPossibly the origin of the matter-antimatter asymmetry of the universe?e?
►Are there additional neutrino species as may Are there additional neutrino species as may be hinted by the LSND experiment?be hinted by the LSND experiment?
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18 Feb. 2005, E.J.Chun, KIAS Workshop for Underground Experiment and Astroparticle Physics, Muju, 2005. 2. 16-19
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Majorana(Majorana( = = cc) or Dirac() or Dirac( cc)?)?L L 0 or 0 or L= 0 L= 0
► Neutrinoless double beNeutrinoless double beta decay (0ta decay (0))
► Beta decayBeta decay
ppnn
nn pp
ppnn
nn pp
e-e-
e-e-
e-e-
mm
e-e-
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18 Feb. 2005, E.J.Chun, KIAS Workshop for Underground Experiment and Astroparticle Physics, Muju, 2005. 2. 16-19
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Neutrino mass patternsNeutrino mass patterns
mm = 0.1-0.5 eV = 0.1-0.5 eV : : QQuasi-uasi-DDegenerate egenerate cosmologiccosmological massal mass – – 200 kg200 kg of isotope of isotope
mm = 0.02-0.05 eV = 0.02-0.05 eV : : IInverted-nverted-HHierarchy ierarchy oror QD with QD with NNormal-ormal-HHierarchy ierarchy atmospheric neutrino massatmospheric neutrino mass – – 1 ton1 ton
mm = 2-5 meV = 2-5 meV : QD, IH, NH : QD, IH, NH solar neutrino masssolar neutrino mass – – 100 tons100 tons
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Tritium beta decay Tritium beta decay mmee
< 2.2 eV < 2.2 eV at Mainz & Troitsk at Mainz & Troitsk
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Cosmolgy Cosmolgy
► Neutrino dark matter (hot)Neutrino dark matter (hot) hh22 = = ii m mii/92.5 eV/92.5 eV► Power spectrum of small scale structure Power spectrum of small scale structure ddFS FS (Gpc) (Gpc) »» 1/m 1/m (eV) (eV)
* current bound : * current bound : ii m mii < 0.2-0.6 eV < 0.2-0.6 eV
* future sensitivity : 0.14 eV (Planck)* future sensitivity : 0.14 eV (Planck)
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( Astrophysics )( Astrophysics ) physics/0411216physics/0411216
► Detection of the GZK neutrinosDetection of the GZK neutrinos (E(E > 10 > 101515 eV), produced from the interactio eV), produced from the interactio
ns of UHECR protons with CMBRns of UHECR protons with CMBR► $10 million to enhance radio-based technol$10 million to enhance radio-based technol
ogies or develop new technologies reaching ogies or develop new technologies reaching 10 x sensitivity.10 x sensitivity.
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( An astrophysical neutrino flux model )( An astrophysical neutrino flux model )
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Neutrino mases and mixingNeutrino mases and mixingll = = I I U Uli li eeiii/2i/2 ii
l = e, l = e, , , and i = 1, 2, 3 and i = 1, 2, 3 three angles: three angles: ijij; three phases: ; three phases: 1,21,2, , ; ;
three masses: three masses: mmii
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00 & & decay and oscillations decay and oscillations
APS 0APS 0 study : hep-ph/0412300 study : hep-ph/0412300
► P(P(ll -> -> kk) = ) =
sinsin2222 sin sin22[1.27[1.27mm22ijij(eV(eV22)L(km)/E(GeV)])L(km)/E(GeV)]
► decay : decay : mmee = [ = [ ii |U |Ueiei||22mmii
22]]11/2/2
►decay : decay : mm = | = |ii U Ueiei22 m mii e eiiii | |
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Oscillation parametersOscillation parameters SK,K2K,SNO,KamLAND,CHOOZSK,K2K,SNO,KamLAND,CHOOZ
► mm222121 = 8.2 = 8.2 ££ 10 10-5-5 eV eV22
1212 = 32.3 = 32.3oo
► || m m223232| = 2.0 | = 2.0 ££ 10 10-3-3 eV eV22
sinsin22222323 > 0.94 > 0.94► sinsin22221313 < 0.11 < 0.11
QD: m0 ¼ m3,2,1NH: NH: mm22
3232 > 0 (m > 0 (m33 > m > m22 > > mm11) ) IH: IH: mm22
3232 < 0 (m < 0 (m22 > m > m11 > > mm33))
+0.6-0.5
+0.6-0.4
+2.7-2.4
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Ranges of mRanges of m
►NH: mNH: m = |[ = |[ m m22SS]]1/21/2 s s1212
22 c c232322
+[+[ m m22AA ] ]1/21/2 s s1313
22 e e-i-i22||
► IH: mIH: m = [ = [ m m22AA]]1/21/2 c c1313
2 2
££[1-4s[1-4s121222cc1212
2 2 sinsin22((22--11)/2])/2]1/2 1/2
►QD: mQD: m=m=m00 |(c |(c121222eeii11+s+s1212
22eeii22)c)c13132 2
+s+s131322||
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Ranges of mRanges of m
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00 and nuclear structure and nuclear structure
► Decay rate of (A, Z) -> (A, Z+2) e+ e+ : 1/TDecay rate of (A, Z) -> (A, Z+2) e+ e+ : 1/T00
1/21/2(A,Z) = (A,Z) =
GG00(E(E00,Z) | M,Z) | M00GTGT – (g – (gVV
22/g/gAA22) M) M00
FF | |22 m m22
► Heidelberg-Moscow Heidelberg-Moscow 7676Ge experiment : Ge experiment : TT00
1/21/2 > 1.9 10 > 1.9 102525 yrs yrs !! mm < 0.55 eV < 0.55 eV
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Nuclear structure issuesNuclear structure issues
► QQuasiparticle uasiparticle RRandom andom PPhase hase AApproximation (10%?)pproximation (10%?)► Shell ModelShell Model► Constraining with other observablesConstraining with other observables► Reducing the uncertainty (factor 2-3 presently) :Reducing the uncertainty (factor 2-3 presently) :
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Future prospectsFuture prospects Bilenky et.al., hep-ph/0402250Bilenky et.al., hep-ph/0402250
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(note) Beta decay : m(note) Beta decay : mee < 0.2 eV at KATRIN < 0.2 eV at KATRIN
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ConclusionsConclusions hep-ph/0412300hep-ph/0412300