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