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

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

DM Capture (for the “vanilla” WIMP) WIMPs thermally relaxed within the star: Distribution WIMP resilience volume  point-source R X  10 9 cm<<R c Equilibrium timescales are short At equilibrium Capture rate C Seminal literature by: Gould, Griest, Press, Raffelt,Salati, Seckel, Spergel … Dark Luminosity “Dark Luminosity” inside the star Energy transport effects: scatter of orbiting DM

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

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

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

WIMPs and the SUN: energy transport  ≈ cm,  = cm 2 [Taoso, FI, 2010] self annihilatingnon annihilating DM annihil. & DM transp o.o.m. smaller nuclear DM transp o.o.m. nuclear

Asymmetric DM and the SUN: energy transport effects [Bottino et al. `02] asymmetric DM can modify solar structure at > % level in the core ≤ cm 3 /s [Taoso, FI et al. `10]

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

Exclusion power using 8 B neutrinos See also [Cumberbatch et al. `10] (helioseismology, weaker diagnostic) [Taoso, FI et al. `10]  B = 25%  B = 5%  B = x 10 6 cm -2 s -1 Benchmark flux [SNO] EXCLUDED! (1pb)

Self-Interacting DM in the Sun Capture of SI-DM Limited by geometrical cross section of DM region (optical limit)  r 2  No sizable effect on solar composition disagreement with [Frandsen & Sarkar `10] [Taoso, FI, et al. `10]

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

Self annihilating DM: compact objects at the Galactic Centre Carbon neutron stars  SI = cm 2 [Moskalenko & Wai `07] [de Lavallaz & Fairbairn `10]  SI = cm 2

White dwarves in Globular Clusters DM profile reconstructed from baryons/stars [Bertone & Fairbairn 08] White dwarfs DENSE and with no intrinsic energy production WD, blackbody approx T *, L *  r *  C *  DM =10 4 GeV/cm 3 (sample stars from the innermost field) GC baryon dominated

SA Inelastic DM (WD in M4)  DM =8x10 2 GeV/cm 3  SI = cm 2 [McCullough & Fairbairn `10] see also [Hooper et al `10]

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

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