Relativistic accretion disks

The Shakura & Sunyaev model is the mostly adopted description of the thermal emission produced by the accretion disk around a black hole and infers rough estimates of the disk luminosity and the black hole mass. More advanced models have been developed in order to account for general relativistic effects, including the role of the black hole spin. My aim is to describe and compare two relativistic disk models, KERRBB and SLIMBH, to show: i) their effect on the fitting process of the Spectral Energy Distribution, and ii) the possible usage to shed light on the geometry of the dusty torus surrounding the AGN central engine