Flavor Physics and Dark Matter in SUSY GUT Models Yudi Santoso - - PowerPoint PPT Presentation

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Flavor Physics and Dark Matter in SUSY GUT Models Yudi Santoso - - PowerPoint PPT Presentation

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Flavor Physics and Dark Matter in SUSY GUT Models Yudi Santoso Based on works with Bhaskar Dutta & Yukihiro Mimura PRD80:095005,2009 PHENO 2010, Madison, 11 th May 2010 1 Supersymmetry Why SUSY? It provides solution to hierarchy problem,

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Flavor Physics and Dark Matter in SUSY GUT Models

Yudi Santoso

Based on works with

Bhaskar Dutta & Yukihiro Mimura

PRD80:095005,2009 PHENO 2010, Madison, 11th May 2010

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Supersymmetry

Why SUSY? It provides solution to hierarchy problem, improves gauge coupling unification, provides dark matter particle. Unsolved problem: How do we understand flavor structure within SUSY? (How SUSY is broken?)

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Flavor & SUSY

Flavor puzzle of SUSY: (without restriction by hand) soft breaking terms allow large flavor changing processes. FCNC can be suppressed by flavor universal SUSY breaking: Universal squarks and sleptons masses

m ˜

U, m ˜ D, m ˜ Q, m˜ L, m ˜ E = Im0.

Universal trilinear coupling coefficents

A = Y A0 (Y = Yukawa).

Nevertheless, nonuniversality still arises through RGE,

⇒ FCNC through radiative correction.

Within SUSY GUT - How the quark sector is related to the lepton sector?

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Bs − ¯ Bs mixing

Large phase is measured: CDF: φs ∈ [0.28, 1.29]

(PRL100 (2008) 161802)

D0 : φs = 0.57+0.30

−0.24(stat)+0.02 −0.07(syst)

(PRL101 (2008) 241801)

Standard Model:

φs = 2βs ≡ 2 arg (−VtsV ∗

tb/VcsV ∗ cb) ≃ 0.04

s i b W W s j b s i b W W s j b

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Bs − ¯ Bs mixing - SUSY

Chargino box diagrams. Double penguin diagrams through heavy Higgs. This is ∝ tan4 β and ∝ 1/m4

A

(Recall also that BR(Bs → µµ) ∝ tan6 β) Define

CBse2iφBs = MSM

12 + MNP 12

MSM

12

then

φs = 2(βs − φBs)

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Neutrino in the GUT-shell

Observation:

θ12 (solar) - large, θ23 (atmospheric) - large, θ13 (reactor)

  • small, and small neutrino masses.

Light neutrinos through seesaw:

Mlight

ν

= f∆L − YνM−1

R Y T ν H0 u2

Seesaw type II I

∆L is an SU(2)L triplet, and f is a Majorana coupling

1 2LL∆L.

Large mixing through Majorana coupling (type II) or Dirac coupling (type I).

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GUT boundary condition

Squark and slepton mass matrices:

M2

˜ F = m2 0[1 − κF UF diag(k1, k2, 1)U† F ]

Minimal type SU(5) :

κL = κDc, UL = UDc, κQ = κU c = κEc = 0

Minimal type SO(10) :

κQ = κU c = κDc, UQ = UU c = UDc, κL = κEc

(To obey proton decay constraint. Dutta, Mimura and Mohapatra, PRL94 (2005) 091804, PRD72 (2005) 075009)

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Neutralino Dark Matter

Direct detection cross section

σ˜

χ0

1−p

≃ 4 πm4

p|(Aufu/mu + Acfc/mc + Atft/mt)

+(Adfd/md + Asfs/ms + Abfb/mb)|2

where, fq ≡ p|mq¯

qq|p/mp, and fu ≃ 0.027; fd ≃ 0.039; fs ≃ 0.36; fc = fb = ft ≃ 0.043 Ad,s,b = g2

2md,s,b

4MW

  • −sin α

cos β Fh m2

h

+ cos α cos β FH m2

H

  • Au,c,t

= g2

2mu,c,t

4MW cos α sin β Fh m2

h

+ sin α sin β FH m2

H

  • 8
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SU(5) mA − µ plane

400 600 800 1000 200 400 600 800 1000 400 600 800 1000 200 400 600 800 1000

mA[GeV] µ[GeV]

2 × 10-8 3 × 1 0-8 . 5 × 1

  • 8

p b 1 2 5 tan β = 40, A0 = 0, m1/2 = 500 GeV, m0 = 500 GeV

400 600 800 1000 200 400 600 800 1000 400 600 800 1000 200 400 600 800 1000

mA[GeV] µ[GeV]

2 × 10-8 3 × 1

  • 8

0.5 × 10-8 pb 1 2 5 tan β = 40, A0 = 0, m1/2 = 500 GeV, m0 = 1 TeV

|2φBs| = 0.5 rad.

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SO(10) mA − µ plane

200 400 600 800 1000 200 400 600 800 1000 200 400 600 800 1000 200 400 600 800 1000

mA[GeV] µ[GeV]

1 × 10-8 2 × 10-8 3 × 10-8 0.5 × 10-8 pb 1 2 5 tan β = 40, A0 = 0, m1/2 = 500 GeV, m0 = 500 GeV

500 1000 1500 200 400 600 800 1000 500 1000 1500 200 400 600 800 1000

mA[GeV] µ[GeV]

1 × 10-8 2 × 10-8 3 × 10-8 0.5 × 10-8 pb 1 2 5 0.05 . 1 tan β = 40, A0 = 0, m1/2 = 800 GeV, m0 = 500 GeV

|2φBs| = 0.5 rad.

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σχ-p × 10-6 pb Br(Bs → µ+µ-) ×10-8

2 5 G e V 500 GeV 750 GeV µ = 1 T e V

SO(10)

tan β = 40, A0 = 0, m0 = 500 GeV, m1/2 = 500 GeV

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σχ-p × 10-6 pb Br(Bs → µ+µ-) ×10-8

2 5 G e V 500 GeV 750 GeV µ = 1 TeV

SU(5)

tan β = 40, A0 = 0, m0 = 500 GeV, m1/2 = 500 GeV

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Conclusion

We have looked at models of SUSY GUT in which

Bs − ¯ Bs mixing phase can be large and with large

neutrino mixing. Combined with other flavor changing constraints and dark matter constraints we found that the funnel region is still allowed by both SU(5) and SO(10), and favored by SU(5). Stronger constraints from upcoming experimental results can provide further hints on the SUSY GUT model.

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