If dark matter is dissipative then the distribution of dark matter within galactic halos can be governed by dissipation, heating and hydrostatic equilibrium. Previous work has shown that a specific model, in the framework of mirror dark matter, can explain several empirical galactic scaling relations. It is shown here that this dynamical halo model implies a quasi-isothermal dark matter density, $\rho (r) = \rho_0 r_0^2/(r^2 + r_0^2)$, where the core radius, $r_0$, scales with disk scale length, $r_D$, via $r_0/{ \rm kpc} = 1.4\left(r_D/{ \rm kpc}\right)$. Additionally, the product $\rho_0 r_0$ is roughly $constant$, i.e. independent of galaxy size (the $constant$ is set by the parameters of the model). The derived dark matter density profile implies that the galactic rotation velocity satisfies the Tully-Fisher relation, $L_B \propto v^{ 3}_{ max}$, where $v_{ max}$ is the maximal rotational velocity. Examples of rotation curves resulting from this dynamics are given.
Categories: astro-ph.GA astro-ph.CO hep-ph