Speaker
Venya Berezinsky
Description
The review of analytic studies of DM-clump production, evolution and destruction is
presented. In the standard scenario of adiabatic and Gaussian fluctuations the clump
formation starts at MD epoch and proceeds in the hierarchical structures when a small
clump belongs to a host clump, this host clump is submerged to bigger one etc. The
formation of density profile $\rho(r)\propto r^{-\beta}$
with $\beta\approx 1.7−1.9$ is accompanied by the tidal
destruction of the clumps. Only a small fraction of clumps survive. Much attention
is given to formation and size of the the core. The role of adiabatic protection of the
core is discussed for the processes of clump destruction in the hierarchical structures and
Milky Way. The minimal clump mass is provided by wiping off the fluctuations during
and after kinetic decoupling and depends on elementary-particle model for DM particles.
The minimal mass can vary in the wide range of values. The boost factor (amplification
of annihilation signal) is discussed. It is concluded that within parameter uncertainties
in the standard adiabatic scenario and especially in non-standard scenarios resulting in
superdense clumps, the annihilation-signal amplification can be large.
