  If the gas in the evolving cosmic halos is dissipating energy (cooling) then
due to the variation of the gravitational potential the dark matter halo also
undergoes a compactification. This is well-known as Adiabatic contraction (AC).
Complementary to the AC we investigate the resulting dynamical behaviour of the
whole system if the backreaction of the AC of DM onto the gas is taken into
account. In order to achieve sufficient high resolution also within the central
halo region, we use a crude fluid approximation for the DM obeying the
adiabatic contraction behaviour. Further, we restrict ourself to spherical
symmetry and vanishing angular momentum of the studied matter configurations.
The computations are done using a first-order Godunov type scheme. Our results
show that the dynamical interaction between gas and DM may lead to significant
shorter collapse times. If the gas cools the dynamical behaviour of the whole
system depends strongly on the shape of the initial density profile. Our
findings indicate that for a certain mass range of halo configurations the
dynamical interaction between gas and DM might be important for the halo
evolution and must be taken into account.
