  We simulate the adiabatic contraction of a dark matter (DM) distribution
during the process of the star formation, paying particular attention to the
phase space distribution of the DM particles after the contraction. Assuming
the initial uniform density and Maxwellian distribution of DM velocities, we
find that the number $n(r)$ of DM particles within the radius $r$ scales like
$n(r) \propto r^{1.5}$, leading to the DM density profile $\rho\propto
r^{-1.5}$, in agreement with the Liouville theorem and previous numerical
studies. At the same time, the number of DM particles $\nu(r)$ with periastra
smaller than $r$ is parametrically larger, $\nu(r) \propto r$, implying that
many particles contributing at any given moment into the density $\rho(r)$ at
small $r$ have very elongated orbits and spend most of their time at distances
larger than $r$. This has implications for the capture of DM by stars in the
process of their formation. As a concrete example we consider the case of
primordial black holes (PBH). We show that accounting for very eccentric orbits
boosts the amount of captured PBH by a factor of up to $2\times 10^3$ depending
on the PBH mass, improving correspondingly the previously derived constraints
on the PBH abundance.
