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

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Concrete ModelConstraintsConstraints from LFVBr(l α → l β γ) = 3α em64πG 2 F M4 η3∑∣i=1The experimental boundsBr(µ → eγ) < 2.4×10 −12Br(τ → µγ) < 4.4×10 −8Br(τ → eγ) < 3.3×10 −8( Mhαi ∗ 2) ∣ 2h i ∣∣∣βiF 2Mη2 Br(l α → l β ν α ν β )where Br(µ → eν µ ν e ) ≃ 1, Br(τ → µν τ ν µ ) ≃ 0.174,Br(τ → eν τ ν e ) ≃ 0.178.→ Yukawa couplings h αi should be small.orSpecial structure of Yukawa matrix.Takashi Toma (IPPP) Internal Seminar 7th June 2013 18 / 34
Concrete ModelConstraintsConstraint from DM Relic DensityThe lightest right-h<strong>and</strong>ed neutrino N 1 is assumed to be DMc<strong>and</strong>idate.The channel: N 1 N 1 → l α l β (t, u-channel)Expansion in terms of v 2 , σv = a+bv 2 +O(v 4 )Fermionic DM is often suppressed by chiral suppression.The annihilation cross section has no s-wave due to chiralsuppression.σv =τ∑α=e|h α1 | 424πM 2 1(M41 +M 4 η)( )M21 +Mη2 4v 2 ∝ v 2→ the Yukawa couplings h αi should be large.Takashi Toma (IPPP) Internal Seminar 7th June 2013 19 / 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 16 and 17: Concrete ModelConstraintsThe parame
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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