time in these systems is shorter than the dynamical times, we restrict ourselves to steady-state configurations that do not include an explicit coupling to hydrodynamics.

In section \[MethodologySection\], we describe how we parametrize the gas configurations surrounding the black hole and how we treat the key physical processes in the radiative transfer. In section \[Results\], we present our results for a series of calculations in which we vary the opening angle of the torus, the amount of gas present, and the accretion disk luminosity. We also examine how our dynamical conclusions are affected by accounting for a clumpy rather than smooth distribution of dust and gas. Finally, in section \[Conclusion\] we present our conclusions.

Methodology {#MethodologySection}
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Initial gas configuration - parameterized, smooth model {#DiskGeometry}
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Although the specific region we are studying is difficult to observe directly, gravito-hydrodynamic simulations [@Hopkins2012-1] provide information about its configuration before the effects of radiative feedback are felt. The gas and stars form a thick disk roughly in vertical hydrostatic equilibrium (our usage of the word “disk” throughout the remainder of this study refers to what is usually labelled as the torus and should not be confused with a reference to the black hole 