2005/11/30 by V. Berezinsky, Veniamin Berezinsky, V. I. Dokuchaev +3 · 2 citations
Physics and Astronomy · #Astronomy #Astrophysics #Bulge #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark matter #Dark matter halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Halo #Physics #Star formation #Stars #Structure formation #astro-ph
paper · pdf · doi:10.1103/physrevd.73.063504
published as Phys.Rev.D73:063504,2006 · 11 pages, 7 figures. Minor changes to reflect referee's comments. Accepted for publication in Phys. Rev. D
arxiv created 2006/02/24 · openalex publication_date 2006/03/08 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
A mass function of small-scale dark matter clumps is calculated in the standard cosmological scenario with an inflationary-produced primordial fluctuation spectrum and with a hierarchical clustering. We take into account the tidal destruction of clumps at early stages of structure formation starting from a time of clump detachment from the Universe expansion. Only a small fraction of these clumps, \ensuremath∼0.1%--0.5%, in each logarithmic mass interval \ensuremathΔlogM\ensuremath∼1 survives the stage of hierarchical clustering. The surviving clumps can be disrupted further in the galaxies by tidal interactions with stars. We performed the detailed calculations of the tidal destruction of clumps by stars in the Galactic bulge and halo and by the Galactic disk itself. It is shown that the Galactic disc provides the dominant contribution to the tidal destruction of small-scale clumps outside the bulge. The results obtained are crucial for calculations of the dark matter annihilation signal in the Galaxy.