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Dark Matter

Dark Matter. Expect Unexpected outside LHC. Jingsheng Li. Introduction. SM is confirmed precisely? NO! Dark Matter is OUT THERE!! SC=SM+more ∟ (New Phy=ptc+int) +unexpected ∟ astrophy effect? ∟ modify gravity?. Outline. Standard Cosmology Evidence for Dark Matter

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Dark Matter

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  1. Dark Matter Expect Unexpected outside LHC Jingsheng Li

  2. Introduction • SM is confirmed precisely? • NO! • Dark Matter is OUT THERE!! • SC=SM+more • ∟(New Phy=ptc+int) +unexpected • ∟astrophy effect? • ∟ modify gravity?

  3. Outline • Standard Cosmology • Evidence for Dark Matter • Relic Density • Candidates • Dark Matter Detection

  4. Standard Cosmology • Smooth Universe • Friedman Eqn • Content ( w=/P, ) • baryon w=0 radiation w=1/3 c.d.m. w=0 c.c. w=-1

  5. A Brief History of Universe

  6. Properties of DM • Dark (rotation curve, gra. lensing) • Cold (Structure formation) • Weakly Interacting(rotation curve, Bullet Cluster) • b/m=1/6 (BBN, CMB, Bullet Cluster 1E0657-558)

  7. Evolution of CDM • Boltzmann Eqn (1+23+4) • Note: • Eq (T>m), freeze out (T<m)

  8. Relic Density

  9. Lee-Weinberg Bound • Anti-baryon • 45GeVL • Scalar DM Higgs exchange, even weaker, expect for Boehm, Fayet (N=2) Lee-Weinberg is good for >GeV range

  10. Candidate VS Test UED w/ KK-parity, LH w/ T-parity, Techni Baryon, monopole, R….

  11. SUSY WIMP • SUSY w/ R-parity provides LSP • Spctrum depends on Mediation Scheme • Hidden Sector • GMSB: gravitino as LSP, cosmo constraint: • NLSP decay, BBN and CMB constraints • Gravity Mediated , decay, BBN constraint • Neutralino as LSP: In Lee-Weinberg bound

  12. Neutralino • Decay channels • univ~10Gyr, set upper bound for Mh2<0.3,lower bound for , upper bound for mint. • Cosmology set upper bound on superpartner, good for LHC?

  13. Axion (non-thermal CDM) • PQ SSBAxion • PQ EB  • Coupling to Nucleon • Red Giant emission bound • SN1987A bound • Oscillation energy • Critical density bound • Search:

  14. Detection • MET • Direct Detection • Indirect Detection

  15. Direct Detection

  16. Indirect Detection

  17. Result from indirect detection • e+ excess beyond prediction10 GeV ~ 100GeV (PAMELA), e+e- excess upto TeV (ATIC) • ATIC: sharp falling @ 600GeVno astrophy explaination • SUSY needs 10TeV for PAMELA • No p- excess • Usual Neutralino can’t explain • Very large <v>, conflicts with required relic density.

  18. Solution? • New interaction to annihilate  • Sommerfeld enhancement (Arkani-Hamed)Breit-Wigner enhancement (Murayama)Nonthermal production (Kumar) • DM decay

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