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In the general accretion disk model theory, the accretion disk surrounding anastronomical object comprises fluid rings obeying Keplerian motion. However, weshould consider relativistic and rotational effects as we close in toward thecenter of accretion disk surrounding spinning compact massive objects such as ablack hole or a neutron star. In this study, we explore the geometry of theinner portion of the accretion disk in the context of Mukhopadhyay's pseudoNewtonian potential approximation for the full general relativity theory. Wefound that the shape of the accretion disk "puffs up" or becomes thicker andthe luminosity of the disk could exceed the Eddington luminosity near thesurface of the compact spinning black hole.

Thick accretion disk and Its super Eddington luminosity around spinning blackholes