asymmetric dark matter and the sun
DESCRIPTION
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 - PowerPoint PPT PresentationTRANSCRIPT
Asymmetric dark matter Asymmetric dark matter
and the Sunand the SunFabio Iocco
Marie Curie fellow atInstitut d’Astrophysique de Paris
Cosmo 2010Univ. of Tokyo, Japan 27/9/2010
Based on arXiv:1005.5711 (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 centerby 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-sourceRX109cm<<Rc
Equilibrium timescales are short
At equilibrium
Capture rate C
Seminal literature by:Gould, Griest, Press, Raffelt,Salati, Seckel, Spergel …
“Dark LuminosityDark Luminosity” inside the star
Energy transport effects:scatter of orbiting DM
The Sun: HE s from DM
[Wikstrom & Edsjo `09]JCAP; arXiv:0903.2986
Where does this take place (efficiently)?Galactic Centeris dense in DM
Little DM in our neighborhood
[Ullio et al. `01, Bertone & Merritt `05]
Scattering and transportCaptured WIMPs orbit
and scatter over long
mean free paths
Star
core
x
xx
x
x
DM particlescan efficiently transport heat inside the core
WIMPs and the SUN:energy transport
≈ 1010 cm, =10-36 cm2
[Taoso, FI, 2010]
self annihilating non annihilating
DM annihil. & DM transpo.o.m. smaller nuclear
DM transpo.o.m. nuclear
Asymmetric DM and the SUN:energy transport effects
[Bottino et al. `02]
asymmetric DM can modifysolar structure at > % level in the core
<sv> ≤ 10-33 cm3/s
[Taoso, FI et al. `10]
The WIMPS and Sun: modifying thermal neutrinos
[Taoso, FI et al. `10]
8B produced innermost than 7Be modified by asymmetric DM
Exclusion powerusing 8B neutrinos
See also [Cumberbatch et al. `10](helioseismology, weaker diagnostic)
[Taoso, FI et al. `10]
B = 25%
B = 5%
B= 5.046 x 106 cm-2s-1
Benchmark flux [SNO]
EXCLUDED!
(1pb)
Self-Interacting DM in the Sun
Capture of SI-DMLimited by geometrical
cross section of DM region(optical limit)
r2
No sizable effecton 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 8B 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=10-43 cm2
[Moskalenko & Wai `07]
[de Lavallaz & Fairbairn `10]
SI=10-41 cm2
WhiteWhite dwarves dwarves in Globular Clustersin Globular Clusters
DM profile reconstructedfrom baryons/stars
[Bertone & Fairbairn 08]
White dwarfs DENSE and with
no intrinsic energy productionWD, blackbody approxT*, L* r* C*
DM=104 GeV/cm3
(sample stars from the innermost field)
GC baryon dominated
SA Inelastic DM (WD in M4)
DM=8x102 GeV/cm3
SI=10-40 cm2
[McCullough & Fairbairn `10]see also [Hooper et al `10]
Going cool: WIMP burning 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 DM burning at the Galactic Centerat the Galactic Center
[Scott, Fairbairn & Edsjo `09]
At the limit of effectiveness
With current upper limits on cross section