The Effect of Toroidal Accretion Disks on the Polarization Spectra of Black Holes

The Standard Model of Black Hole Accretion Disks consists of a geometrically thin, optically thick disk whose inner edge truncates at the ISCO. While this model is widely used and can describe a large body of observational data, it is limited to systems with an accretion rate between a few percent and a few tens of percent of the Eddington Limit. Above this threshold, radiation pressure within the disk surely causes it to develop non-zero scale height. In this talk, I will introduce a phenomenological model of a toroidal accretion disk, discuss its implementation into the raytracing code of H. Krawczynski, and review my results for the thermal and Comptonized emission in this geometry. I will also briefly discuss my ongoing collaboration with M. Liska at Harvard, whereby I am implementing the output of the GRMHD simulation of a misaligned disk into the raytracing code.