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Probing neutrino flavor transition mechanism with ultrahigh energy
astrophysical neutrinos
Probing neutrino flavor transition mechanism with ultrahigh energy
astrophysical neutrinos
賴光昶賴光昶長庚大學通識中心長庚大學通識中心
賴光昶賴光昶長庚大學通識中心長庚大學通識中心
2014 海峡两岸粒子物理与宇宙学研讨会
黃山,安徽, May 9th, 2014
KCL, T.-C. Liu and G.-L. Lin, PRD 82, 103003KCL, T.-C. Liu and G.-L. Lin, PRD 82, 103003KCL, T.-C. Liu and G.-L. Lin, PRD 89, 033002KCL, T.-C. Liu and G.-L. Lin, PRD 89, 033002
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Astrophysical neutrinoAstrophysical neutrino
Neutrino flavor transitionNeutrino flavor transition
Neutrino signals in neutrino telescopesNeutrino signals in neutrino telescopes
Test of transition modelsTest of transition models
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ErnieErnieErnieErnie
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Bert, Bert, 1.04PeV1.04PeV Ernie, Ernie, 1.14PeV1.14PeV
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Astrophysical Astrophysical neutrinoneutrino
Astrophysical Astrophysical neutrinoneutrino
““AstrophysicalAstrophysical”” means means
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QQ-representation-representation
Standard oscillationStandard oscillation
Neutrino decayNeutrino decay
QQuantum decoherenceuantum decoherence
Pseudo-Dirac neutrinoPseudo-Dirac neutrino
Flavor transitionFlavor transitionFlavor transitionFlavor transition
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Q-representationQ-representationQ-representationQ-representation
neutrino on Earthneutrino on Earth→φ=Pφ→φ=Pφ00←←neutrino at the sourceneutrino at the sourceφφ00==((φφ00((νe), ), φφ00((νμ), ), φφ00((ντ))=1/3))=1/3VV11+a+aVV22+b+bVV33
φφ==ϰϰVV11++ϱϱVV22++λλVV33
((ϰϰ, , ϱϱ, , λλ))TT==QQ((11//3, a, b3, a, b))TT
⇒⇒Q≡AQ≡A-1-1PAPA
Tri-bimaximal matrix, eigenvectors of TBMTri-bimaximal matrix, eigenvectors of TBM::
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Q-representationQ-representationQ-representationQ-representation
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Standard oscillationStandard oscillationStandard oscillationStandard oscillation
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Neutrino decayNeutrino decayNeutrino decayNeutrino decay
NormalNormalhierarchyhierarchy
InvertedInvertedhierarchyhierarchy
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Neutrino decayNeutrino decayNeutrino decayNeutrino decayThe heaviest and The heaviest and
middle states decay middle states decay
into the lightest into the lightest
one(j=1 or 3).-one(j=1 or 3).-dec1dec1
The heaviest state The heaviest state
decays into the middle decays into the middle
and lightest ones.-and lightest ones.-dec2dec2{{
εε11==coscos2ϑ2ϑ2323--((√√2/3)sin2/3)sinϑϑ1313, , εε22=(1/2)=(1/2)coscos2ϑ2ϑ2323--εε11
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Quantum Quantum decoherencedecoherence
Quantum Quantum decoherencedecoherence
distance dependentdistance dependent
γγ→0 or →0 or d→d→∞∞, , QQdcdc=Q=Qoscosc
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∆∆mmii22: the mass-squared difference between active and sterile states.: the mass-squared difference between active and sterile states.
Pseudo-Dirac Pseudo-Dirac neutrinoneutrino
Pseudo-Dirac Pseudo-Dirac neutrinoneutrino
∆∆mmii22 =∆m =∆m22
In the limit of L(z)/4EIn the limit of L(z)/4Eνν≫1/≫1/∆m∆mii22, , QQpdpd=1/2 =1/2
QQoscosc
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Neutrino eventsNeutrino eventsNeutrino eventsNeutrino events
125m corresponds to the decay 125m corresponds to the decay length of a 2.5 PeV tau lepton.-length of a 2.5 PeV tau lepton.-dist. between stringsdist. between strings ≈ ≈1km corresponds to the decay 1km corresponds to the decay length of a 25 PeV tau lepton.-length of a 25 PeV tau lepton.-size of IceCubesize of IceCube1054.51541054.5154
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ObservablesObservablesObservablesObservables
Case I:Eν<33PeV
Case II:Eν>33PeV
RI=ϕ(νμ)/(ϕ(νe)+ϕ(ντ))SI= ϕ(νe)/ϕ(ντ)
RII=ϕ(νe)/(ϕ(νμ)+ϕ(ντ))
SII= ϕ(νμ)/ϕ(ντ)
RI: track-to-shower ratio; RII:shower-to-track ratio
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ObservablesObservablesObservablesObservables
ϕ0=(ϕ(νe), ϕ(νμ), ϕ(ντ))=1/3 V1+aV2+bV3.
for non-ντ sources, a=-1/3+b and let RII≡R.
flux conservation assumed
For pion and damped-muon sources
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Statistical analysisStatistical analysisStatistical analysisStatistical analysisWe consider: We consider: • i=π, only pion sourcei=π, only pion source• i=π and µ, both pion i=π and µ, both pion and damped-muon and damped-muon sourcesource• σσ=10% assumed=10% assumed
G. Fogli, et al., PRD 86, G. Fogli, et al., PRD 86, 013012013012
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Statistical analysisStatistical analysisStatistical analysisStatistical analysis
Legend:Legend:
• ✕✕: oscillation: oscillation
• ▵▵: dec1-n, : dec1-n, ▴▴:dec1-i:dec1-i
• ○○ , , ◇◇, , ⃞⃞: dec2-n: dec2-n
• ••, , ◆◆, , ▪▪: dec2-i: dec2-i
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Pion sourcePion sourcePion sourcePion source
11σ σ regionregion 33σ σ regionregion
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Pion sourcePion sourcePion sourcePion source
11σ σ regionregion 33σ σ regionregion
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Pion sourcePion sourcePion sourcePion source11σ σ regionregion 33σ σ regionregion
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Pion and Muon Pion and Muon sourcessources
Pion and Muon Pion and Muon sourcessources
11σ σ regionregion 33σ σ regionregion
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Pion and Muon Pion and Muon sourcessources
Pion and Muon Pion and Muon sourcessources
11σ σ regionregion 33σ σ regionregion
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Pion and Muon Pion and Muon sourcessources
Pion and Muon Pion and Muon sourcessources
11σ σ regionregion 33σ σ regionregion
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SummarySummarySummarySummary
Neutrino astronomy has begun.Neutrino astronomy has begun.
28 astrophysical events observed28 astrophysical events observed
Flavor transitions can be probed:Flavor transitions can be probed:
QQ-representation -representation
Observable definedObservable defined
𝜒𝜒22-analysis performed-analysis performed