1 / 13

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

elvis
Download Presentation

S uper WIMP Dark matter

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related