Abstract
The enhancement of the annihilation signal due to Dark Matter (DM) clumpiness in the Galactic halo, valid for arbitrary DM particles, is described. The mass spectrum of small-scale DM clumps with M≤103M⊙ is calculated with tidal destruction of the clumps taken into account within the hierarchical model of clump structure. The mass distribution of the clumps has a cutoff at Mmin due to diffusion of DM particles out of a fluctuation and free streaming. In the case of neutralino (considered as a pure bino) being a DM particle, Mmin∼108M⊙. The evolution of the density profile in a DM clump does not result in singularity, because of formation of the core under the influence of tidal interaction. The number density of clumps as a function of their mass, radius, and distance to the Galactic center is presented.
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