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Asymmetric dark matter and the Sun

Asymmetric dark matter and the Sun. Fabio Iocco Marie Curie fellow at Institut d’Astrophysique de Paris. Based on arXiv:1005.5711 (PRD in press) Taoso, FI, Meynet, Bertone, Eggenberger. Cosmo 2010 Univ. of Tokyo, Japan 27/9/2010. Scattering and capture. Captured WIMPs accumulate

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Asymmetric dark matter and the Sun

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  1. Asymmetric dark matter and the Sun Fabio Iocco Marie Curie fellow at Institut d’Astrophysique de Paris Based on arXiv:1005.5711 (PRD in press) Taoso, FI, Meynet, Bertone, Eggenberger Cosmo 2010 Univ. of Tokyo, Japan 27/9/2010

  2. Scattering and capture Captured WIMPs accumulate inside the star, thermalize Halo WIMPs are captured X and “sink” to the center by scattering off the gas of the star

  3. DM Capture(for the “vanilla” WIMP) “Dark Luminosity” inside the star Capture rate C At equilibrium WIMPs thermally relaxed within the star: Distribution Energy transport effects: scatter of orbiting DM WIMP resilience volume  point-source RX109cm<<Rc Equilibrium timescales are short Seminal literature by: Gould, Griest, Press, Raffelt,Salati, Seckel, Spergel …

  4. The Sun: HE s from DM [Wikstrom & Edsjo `09] JCAP; arXiv:0903.2986

  5. Where does this take place (efficiently)? Galactic Center is dense in DM Little DM in our neighborhood [Ullio et al. `01, Bertone & Merritt `05]

  6. Scattering and transport Captured WIMPs orbit and scatter over long mean free paths Star x x x x core x DM particles can efficiently transport heat inside the core

  7. WIMPs and the SUN:energy transport self annihilating non annihilating DM annihil. & DM transp o.o.m. smaller nuclear DM transp o.o.m. nuclear lc ≈ 1010 cm, s =10-36 cm2 [Taoso, FI, 2010]

  8. Asymmetric DM and the SUN:energy transport effects <sv> ≤ 10-33 cm3/s [Bottino et al. `02] asymmetric DM can modify solar structure at > % level in the core [Taoso, FI et al. `10]

  9. The WIMPS and Sun: modifying thermal neutrinos 8B n produced innermost than 7Be n modified by asymmetric DM [Taoso, FI et al. `10]

  10. Exclusion powerusing 8B neutrinos Benchmark n flux [SNO] fB= 5.046 x 106 cm-2s-1 EXCLUDED! DfB = 5% DfB = 25% (1pb) [Taoso, FI et al. `10] See also [Cumberbatch et al. `10] (helioseismology, weaker diagnostic)

  11. Self-Interacting DM in the Sun Capture of SI-DM Limited by geometrical cross section of DM region (optical limit) pr2c No sizable effect on solar composition disagreement with [Frandsen & Sarkar `10] [Taoso, FI, et al. `10]

  12. Conclusions Self annihilating DM can not modify the structure of the Sun Non annihilating DM canmodify the structure of the Sun  Non annihilating DM induces variation on 8B neutrino flux  Competitive constraints on SD cross section (low masses)  More to be addressesd with other type of stars in other environs

  13. Self annihilating DM:compact objects at the Galactic Centre Carbon neutron stars sSI=10-41 cm2 [de Lavallaz & Fairbairn `10] sSI=10-43 cm2 [Moskalenko & Wai `07]

  14. Whitedwarvesin GlobularClusters White dwarfs DENSE and with no intrinsic energy production WD, blackbody approx T*, L* r*  C* rDM=104 GeV/cm3 DM profile reconstructed from baryons/stars (sample stars from the innermost field) GC baryon dominated [Bertone & Fairbairn 08]

  15. SA Inelastic DM (WD in M4) rDM=8x102 GeV/cm3 sSI=10-40 cm2 [McCullough & Fairbairn `10] see also [Hooper et al `10]

  16. Going cool:WIMPburning (stars have negative specific heat) [Iocco et al. 08] [Fairbairn et al. 08] Similar semi-analytical solutions with “cosmions”: Salati & Silk 89

  17. DM burning at the Galactic Center At the limit of effectiveness With current upper limits on cross section [Scott, Fairbairn & Edsjo `09]

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