Black hole formation in the context of dissipative dark matter
  Black holes with masses of $\rm 10^6-10^9~M_{\odot}$ dwell in the centers of
most galaxies, but their formation mechanisms are not well known. A subdominant
dissipative component of dark matter with similar properties to the ordinary
baryons, known as mirror dark matter, may collapse to form massive black holes
during the epoch of first galaxies formation. In this study, we explore the
possibility of massive black hole formation via this alternative scenario. We
perform three-dimensional cosmological simulations for four distinct halos and
compare their thermal, chemical and dynamical evolution in both the ordinary
and the mirror sectors. We find that the collapse of halos is significantly
delayed in the mirror sector due to the lack of $\rm H_2$ cooling and only
halos with masses above $ \rm \geq 10^7~ M_{\odot}$ are formed. Overall, the
mass inflow rates are $\rm \geq 10^{-2}~M_{\odot}/yr$ and there is less
fragmentation. This suggests that the conditions for the formation of massive
objects, including black holes, are more favorable in the mirror sector.
