TeV Scale Seesaw with Loop Induced

Transcription

1 TeV Scale Seesaw with Loop Induced Dirac Mass Term and Dark kmtt Matter from U(1) B L Gauge Symmetry Breaking Takehiro Nabeshima University of Toyama S. Kanemura, T.N., H. Sugiyama, Phys. Lett. B703:66-70 S. Kanemura, T.N., H. Sugiyama, Phys. Rev. D 85, Toyama workshop Feb 2012

2 Contents 1.Introduction 2.Model 3.Neutrino mass and dark matter 4.Phenomenology 5.Conclusion

3 1.Introduction WIMP DM: M DM ~ O( )GeV U(1)x breaking at (1-10)TeV; 10)TeV; naturally explain the dark matter mass. Neutrino must have tiny masses ( O(0.1)eV) Right handed neutrino and U(1)x; naturally explain neutrino masses at O(1-10)TeV physics at loop level. TeV scale physics cloud explain mass of fdark matter and tiny neutrino masses.

4 1.Introduction WIMP DM: M DM ~ O( )GeV. U(1)x breaking at (1-10)TeV; 10)TeV; naturally explain the dark matter mass. Neutrino must have tiny masses ( O(0.1)eV). Right handed neutrino and U(1)x; naturally explain neutrino masses at O(1-10)TeV physics at loop level. TeV scale physics cloud explain mass of fdark matter and tiny neutrino masses. We consider this case

5 1.Introduction neutrino masses ν R Aoki, Kanemura, Seto(2008) Φ Φ M ~ O(1) TeV y ~ O(10-6 ) M ~ O(1) TeV y ~ O(10-4 ) M ~ O(1) TeV y ~ O(1)

6 1.Introduction neutrino masses ν R Aoki, Kanemura, Seto(2008) Φ Φ M ~ O(1) TeV y ~ O(10-6 ) Φ M ~ O(1) TeV y ~ O(10-4 ) Φ M ~ O(1) TeV y ~ O(1) Φ ν R ν R M ~ O(1) TeV y ~ O( )

7 1.Introduction neutrino masses ν R Aoki, Kanemura, Seto(2008) Φ Φ M ~ O(1) TeV y ~ O(10-6 ) Φ M ~ O(1) TeV y ~ O(10-4 ) Φ M ~ O(1) TeV y ~ O(1) Φ ν R ν R M ~ O(1) TeV y ~ O( ) We consider this case

8 2.Model SU(3) C SU(2) U(1) I Y U(1) B-L new matter particle: -B-L Higgs σ 12 1,2 -Right handed neutrino ν R -SU(2) I singlet scalar s -SU(2) I doublet scalar η 1,2 - SU(2) I singlet chiral fermion Ψ R, L Half unit of U(1) B-L charge U(1) B-L protect: Tree-level LΦν R Majorana mass of ν R Dirac mass of Ψ

9 2.Model U(1) B-L breaking R, R and L Electroweak symmetry breaking s and Physical state: h,h,s1,s2,η ± Remnant global U(1) DM remains on half unit of U(1) B-L charged particles after SSB of U(1) B-L. U(1) DM guarantees the stability of dark matter. We assume that the Ψ 1 is the lightest U(1) DM particle case.

10 3.Neutrino mass and dark matter U(1) B-L Masses of neutrino EW <Φ> <Φ> Φ s s ν R s R L L R L ν R <σ> <Φ> <σ> R s <σ> <σ> <σ> <σ> ν R L R R L <σ> s <Φ> The O(0.1) ev neutrino masses can be naturally deduced from TeV scale physics.

11 3.Neutrino mass and dark matter LFV constraint μ f η ± Ψ f γ Relic abundance of Ψ 1 Ψ 1 σ φ y y f e f Experimental upper bound: BR(μ e,γ) < J. Adam et al.(2011) Our model can be satisfied this value. M h =120GeV M H =140GeV cosα=1/ 2 Ψ 1 f Direct detection of Ψ 1 Ψ 1 Kanemura, Seto and Shimomura (2011) Ψ 1 Experimental bound at m DM ~ 57GeV(XENON100): Z = cm 2 E. Aprile et al. (2011) Okada and Seto (2010) N N Our model can be satisfied this value.

12 3.Neutrino mass and dark matter Parameter set Z neutrino oscillation LFV LEP DM abundance DM direct detection 1TeV Ψ 2 Normal Hierarchy, Tri-bi maximal f ij = h ij = M R = 250 GeV, M Ψ1 = 57.0 GeV, M Ψ2 = 800 GeV M S1 = 200 GeV, M S2 = 300 GeV, M h = 120 GeV, M H = 140 GeV, M η ±= 280 GeV, cosθ= 0.05, cosα=1/ 2, /, g B-L =0.2, M Z =2000GeV, v φ =246 GeV, v σ = 5 TeV 100 GeV h H ν R 1,2 S 2 η ± S 1 Ψ 1 (DM)

13 4.Phenomenology (Z x,x) BR Physics of Z Branching ratio of Z (Z XX) (B-L charge) 2 Z decay into l + l invisible about 30% qq Z production cross section ν R ν R at the LHC for s = 14 TeV, Ψ 1 Ψ 1 Ψ 2 Ψ 2 M Z = 2000 GeV and g B-L = M Z (GeV) then 70 pb. L. Basso, A. Belyaev, S.Moretti and C. H. Shepherd Themistocleous (2009) Our model can be tested by the Our model can be tested by the measuring decay of the Z

14 4.Phenomenology Physics of ν R ν R are light masses (O(100) GeV) and not stable. ν R W + j j ν R are produced about 1200 pair from decay of 7000 Z at the LHC for s = 14 TeV with 100 fb -1 data. The mass of ν R can be reconstructed by jjl ± l

15 4.Phenomenology Physics of Higgs boson mixing angle ge betweenb-lhiggs σ and SMHiggs Φ α~π/4 for the thermal abundance of Ψ 1. Γ(h x,x)~ Γ(H x,x)~ Γ(h SM x,x)/2 Two SM-like Higgs bosons whose masses are O(100) GeV with a about half width.

16 1TeV Z U(1) B-L U(1) DM U(1) DM 100 GeV 0.1eV EWSB h ν 1,2 R Maximal H mixing Type 1 like 2-loop seesaw 1-loop neutrino Dirac Yukawa Ψ 2 Ψ 1 (DM) S 2 η ± S 1

17 5.Conclusion 1 We consider the TeV scale seesaw model in which U(1) B L gauge symmetry can be the common origin of neutrino masses, the dark matter mass, and stability of the dark matter. 2 Our model is compatible with current experiment data. 3 Our model can be tested by the measuring decay of the Z boson. 4 The light ν R (O(100)GeV) can be tested at the LHC. 5 Our model predict two SM-like Higgs bosons whose masses are O(100) GeV with about half width. 6 If we assume U(1) B L gauge symmetry at the TeV scale, we can explain li masses of neutrino and ddark matter.

18 Back up

19 Anomaly Same of all B L particle contribution: [U(1) B L ] 3 2 U(1) B L 11 U(1) B L anomaly is not cancel in our model It would be resolved by some heavy singlet fermions with appropriate B L charge. For example; Right hand: 1 9, 1/2 14,/, 1/3 9 left hand: 3/2 14, 5/3 9

20 U(1) B-L breaking ラグランジアン - U(1) B-L Remnant global U(1) DM remains on half unit of U(1) B-L charged particles after ate SSB of U(1) B-L. U(1) DM guarantee stability of dark matter. We consider that the Ψ 1 is lightest U(1) DM particle case.

21 3.Neutrino mass and dark matter LFV constraint η ± γ μ f Ψ f e Experimental upper bound: BR(μ e,γ) < J. Adam et al.(2011) For our parameter set, it is evaluated as BR(μ e,γ) = O f i l b d Our parameter set safety current experimental upper bound but could be within future experimental reach.

22 3.Neutrino mass and dark matter Relic abundance of Ψ 1 f e Ψ 1 LΨη coupling is small η + due to LFV constraint Ψ 1 f e Ψ 1 f σ φ ΨΨσ coupling ~O(0.01) 01) Ψ 1 y y f f but resonance can be used. Mixing between B-L Higgs σ and SM Higgs Φ is essentially important.

23 3.Neutrino mass and dark matter Relic abundance of Ψ 1 Okada and Seto (2010) Kanemura, Seto and Shimomura (2011) Ψ 1 y σ φ y f f M h =120GeV M H =140GeV cosα~1/ 2 Ψ 1 f Ψ 1 is consistent with WMAP data at the M Ψ1 = 57.0 GeV.

24 3.Neutrino mass and dark matter Direct detection of Ψ 1 y Ψ 1 Ψ 1 σ N φ y f N Ψ 1 Ψ 1 Z N N Experimental bound (XENON100): = cm 2 E. Aprile et al. (2011) For our parameter set, it is evaluated as = cm 2 Our parameter set safety current experimental bound but could be within future experimental reach.

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