Dissipative dark matter halos: The steady state solution II

Understand

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.