  Neutralino annihilation in the Galactic halo is the most definite
observational signature proposed for indirect registration of the SUSY Dark
Matter (DM) candidate particles. The corresponding annihilation signal (in the
form of gamma-rays, positrons and antiprotons) may be boosted for one or three
orders of magnitude due to the clustering of cold DM particles into the
small-scale and very dense self-gravitating clumps. We discuss the formation of
these clumps from the initial density perturbations and their successive fate
in the Galactic halo. Only a small fraction of these clumps, $\sim0.1$%, in
each logarithmic mass interval $\Delta\log M\sim1$ survives the stage of
hierarchical clustering. We calculate the probability of surviving the remnants
of dark matter clumps in the Galaxy by modelling the tidal destruction of the
small-scale clumps by the Galactic disk and stars. It is demonstrated that a
substantial fraction of clump remnants may survive through the tidal
destruction during the lifetime of the Galaxy. The resulting mass spectrum of
survived clumps is extended down to the mass of the core of the cosmologically
produced clumps with a minimal mass. The survived dense remnants of tidally
destructed clumps provide an amplification (boosting) of the annihilation
signal with respect to the diffuse DM in the Galactic halo. We describe the
anisotropy of clump distribution caused by the tidal destruction of clumps in
the Galactic disk.
