Yury Eroshenko

Small-scale clumps in the galactic halo and dark matter annihilation

Production of small-scale DM clumps is studied in the standard cosmological scenario with an inflation-produced primeval fluctuation spectrum. Special attention is given to three following problems: (i) The mass spectrum of small-scale clumps with

Destruction of small-scale dark matter clumps in the hierarchical structures and galaxies

M \lesssim 10^3 M_{\odot}

Remnants of dark matter clumps

is calculated with tidal destruction of the clumps taken into account within the hierarchical model of clump structure. Only 0.1 - 0.5% of small clumps survive the stage of tidal destruction in each logarithmic mass interval

Anisotropy of dark matter annihilation with respect to the Galactic plane

\Delta\ln M\sim1

Accretion with back reaction

. (ii) The mass distribution of clumps has a cutoff at

The phantom shell around a black hole and global geometry

M_{\rm min}

Phantom energy accretion onto black hole

due to diffusion of DM particles out of a fluctuation and free streaming at later stage.

Small‐scale dark matter clumps in the galactic halo

M_{\rm min}

ON THE THEORY OF SPHERICALLY SYMMETRIC THIN SHELLS IN CONFORMAL GRAVITY

is a model dependent quantity. In the case the neutralino, considered as a pure bino, is a DM particle,

SUSY dark matter annihilation in the Galactic halo

M_{\rm min} \sim 10^{-8} M_{\odot}