  Mirror dark matter, and other similar dissipative dark matter candidates,
need an energy source to stabilize dark matter halos in spiral galaxies. It has
been suggested previously that ordinary supernovae can potentially supply the
required energy. By matching the energy supplied to the halo from supernovae to
that lost due to radiative cooling, we here derive a rough scaling relation,
$R_{SN} \propto \rho_0 r_0^2$ ($R_{SN}$ is the supernova rate and $\rho_0, \
r_0$ the dark matter central density and core radius). Such a relation is
consistent with dark matter properties inferred from studies of spiral galaxies
with halo masses larger than $3\times 10^{11} M_\odot$. We speculate that other
observed galaxy regularities might be explained within the framework of such
dissipative dark matter.
