Radiative Neutrino Mass Generation and Dark Matter - Institute for ...

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Concrete ModelConstraintsThe parameters are constrained by various aspects.<strong>Neutrino</strong> mass scale m ν ∼ 10 −1 eV<strong>Neutrino</strong> mixingU T PMNS m νU PMNS = diag(m 1 ,m 2 ,m 3 )Lepton flavor violation (LFV)µ → eγ : Br(µ → eγ) ≤ 2.4×10 −12 → 5.7×10 −13 (now)µ → 3e?Thermal relic density of DM· N 1 is assumed to be DM here.· Leptophilic DM.· degenerated with N 2 .Takashi Toma (IPPP) Internal Seminar 7th June 2013 16 / 34
Concrete ModelConstraintsTo derive the neutrino mass scale(λ 5 h 210 −11 ∼ M √ )i ∆m 2〈φ〉 0.05 eVThe structure of the neutrino mass matrix is determined by theYukawa matrix h αi .The flavor structure:⎛ ⎞ǫ 1 ǫ 2 h 3′h αi = ⎝ h 1 h 2 h 3⎠, ǫ i ≪ h ih 1 h 2 −h 3ǫ i are understood as deviations from the Tri-bimaximal mixing.→ sin 2 θ 12 = 1 3 +ǫ, sin2 θ 23 = 1 2 +ǫ′ , sin 2 θ 13 = 0+ǫ ′′ .U T PMNS m νU PMNS = diag(m 1 ,m 2 ,m 3 )Takashi Toma (IPPP) Internal Seminar 7th June 2013 17 / 34
Page 2: OutlineOutline1 Introduction2 Neutr
Page 7: Neutrino Mass GenerationExamples of
Page 10 and 11: Dark MatterNature of DM· stable (o
Page 12 and 13: Dark MatterNon-thermal ProductionNo
Page 14 and 15: Concrete ModelInteractions and Neut
Page 18 and 19: Concrete ModelConstraintsConstraint
Page 20 and 21: Concrete ModelCoannihilation of DMC
Page 22 and 23: Concrete ModelDirect Detection of D
Page 28 and 29: Extensions of Radiative Seesaw1. Su
Page 30 and 31: Extensions of Radiative Seesaw2. Fl
Page 32 and 33: SummarySummary1 The SM should be ex
Page 34: Thank you for your attention!Takash

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