 Vertical structure of an astrophysical disk

The vertical structure of an astrophysical disk describes how mass density, pressure and temperature vary away from its midplane. For a thin, centrally dominated gas layer, hydrostatic equilibrium gives $dp/dz=-\rho {\Omega }_z^{2}z$. An isothermal ideal gas has $p=c_s^2\rho$, producing a Gaussian density profile with disk scale height $H=c_s/{\Omega }_z$. Disk self-gravity or magnetic support changes that balance.^[ref]