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S uper WIMP Dark matter

S uper WIMP Dark matter. Gravitino from Slepton and Sneutrino Decays. Shufang Su • U. of Arizona. J. Feng, F. Takayama, S. Su Hep-ph/0404198. Outline. -. SWIMP dark matter and gravitino LSP Late time energy injection and BBN Slepton and sneutrino NLSP

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S uper WIMP Dark matter

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  1. SuperWIMP Dark matter Gravitino from Slepton and Sneutrino Decays Shufang Su • U. of Arizona J. Feng, F. Takayama, S. Su Hep-ph/0404198

  2. Outline - • SWIMP dark matter and gravitino LSP • Late time energy injection and BBN • Slepton and sneutrino NLSP • Dominant two body EM decay l ! l+G • Subdominant 3-body hadronic decay • Viable parameter space • Conclusion ~

  3. ~ • thG v-1  (gravitional coupling)-2 • (comparig to WIMP of weak coupling strength) • vtoo small • thG too big, overclose the Universe ~ Why gravitino not considered as CDM usually? - However, gravitino can get relic density by other means SuperWIMP

  4. WIMP  SWIMP + SM particle - FRT hep-ph/0302215, 0306024 WIMP 104 s  t  108 s SWIMP SM • Gravitino LSP • LKK graviton 106

  5. ~ SWIMP: G (LSP) WIMP: NLSP mG» mNLSP ~ NLSP  G + SM particles SWIMP and SUSY WIMP - • SUSY case ~ Ellis et. al., hep-ph/0312262 104 s  t  108 s

  6. SWIMP = mG/mNLSP thNLSP ~ Different approach to gravitino superWIMP - ~ NLSP  G + SM particles fix SWIMP = 0.23

  7. EM, had energy injection: EM,had=EM,had BEM,had YNLSP » mNLSP-mG Late time energy injection and BBN - /10-10 = 6.1 0.4 ? Fields, Sarkar, PDG (2002)

  8. EM and Had BBN constraints - EM BBN constraints had BBN constraints EM BBN Cyburt, Ellis, Fields and Olive, PRD 67, 103521 (2003) Kawasaki, Kohri and Moroi, astro-ph/0402490

  9. ~ ~ ~ l  G + l, ! G +  ~ Slepton NLSP lifetime and EM injection - Decay lifetime (sec) EM energy injection EM (GeV)

  10. ~ ~ ~ ~ ~ ~ l lZG,WG, !ZG, lWG Hadronic decay branching ratio - meson contribution mNLSP

  11. Viable Parameter space - 200 GeV · m · 400 » 1500 GeV mG¸ 200 GeV  m · 80 » 300 GeV ~ negligible EM BBN constraints

  12. Conclusions - • SuperWIMP is possible candidate for dark matter • SUSY models: gravitino LSP (SWIMP) slepton NLSP (WIMP) • Constraints from BBN: EM injection and hadronic injection need updated studies of BBN constraints on hadronic/EM injection • Favored mass region: (enlarged if SWIMP<0.23) • Sneutrino: m  80-300 GeV m 100 GeV • Charged R:200 GeV · m · 1500 GeV, mG¸ 200 GeV 500 GeV mR • Rich collider phenomenology(no direct/indirect DM signal) • Charged slepton:highly ionizing track • Sneutrino:missing energy ~ ~ ~ ~ ~

  13. ~ ~ ~ ~ ~ G G G G G • Decay life time  mpl • SM energy distribution  mG  SUSY breaking scale NLSP SM NLSP SM ~ SM NLSP SM NLSP SM NLSP

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