accretion disk, which is unresolved at our scales of interest). The puffiness of the disk in the @Hopkins2012-1 simulations is to some extent determined by the sub-grids turbulent velocity dispersion when strong stellar feedback in the ISM is included, but also by bending modes (firehose instabilities) driven by resolved velocities when less stellar feedback is included. While further accretion of the gas at this scale will rely on non-axisymmetric torques, we first adopt a simple axisymmetric, hydrostatic disk model analogous to one used in @Hopkins2012-1. This parametrization captures the key features of the gas configuration seen in the hydrodynamics simulations, but allows us greater control over free parameters and removes unnecessary complications in our attempt to isolate the effects of the radiation. Such a parametrization also allows us to systematically introduce clumpiness into the gas for certain calculations (which, among other effects, breaks axisymmetry), as will be described in section \[ClumpySetup\]

The vertical structure of the smooth disk model may be calculated by solving the equation of hydrostatic equilibrium in the normal ($z$) direction, assuming an isothermal equation of state with effective sound speed $c_s$ set by both the resolved and sub-grid velocity dispersion, along with any contribution from the 