Dissipative dark matter halos: The steady state solution II
  Within the mirror dark matter model and dissipative dark matter models in
general, halos around galaxies with active star formation (including spirals
and gas rich dwarfs) are dynamical: they expand and contract in response to
heating and cooling processes. Ordinary Type II supernovae (SN) can provide the
dominant heat source, possible if kinetic mixing interaction exists with
strength $\epsilon \sim 10^{-9} - 10^{-10}$. Dissipative dark matter halos can
be modelled as a fluid governed by Euler's equations. Around sufficiently
isolated and unperturbed galaxies the halo can relax to a steady state
configuration, where heating and cooling rates locally balance and hydrostatic
equilibrium prevails. These steady state conditions can be solved to derive the
physical properties, including the halo density and temperature profiles, for
model galaxies. Here, we have considered idealized spherically symmetric
galaxies within the mirror dark particle model, as in the earlier paper [paper
I, arXiv:1707.02528], but we have assumed that the local halo heating in the SN
vicinity dominates over radiative sources. With this assumption, physically
interesting steady state solutions arise which we compute for a representative
range of model galaxies. The end result is a rather simple description of the
dark matter halo around idealized spherically symmetric systems, characterized
in principle by only one parameter, with physical properties that closely
resemble the empirical properties of disk galaxies.
