Description of pseudo-Newtonian potential for the relativistic accretion disks around Kerr black holes

We present a pseudo-Newtonian potential for accretion disk modeling around a rotating black hole. This potential can describe the general relativistic effects on the accretion disk. As the inclusion of rotation in a proper way is very important at the inner edge of the 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.