Description of Pseudo-Newtonian Potential for the Relativistic Accretion Disk around Kerr Black Holes

Abstract

We present a pseudo-Newtonian potential for accretion disk modeling around the rotating black holes. This potential can describe the general relativistic effects on accretion disk. As the inclusion of rotation in a proper way is very important at an inner edge of disk the potential is derived from the Kerr metric. This potential can reproduce all the essential properties of general relativity within 10% error even for rapidly rotating black holes.

5 Latex pages including 1 figure. Version to appear in Astrophysical Journal, V-581, N-1, December 10, 2002

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