  Here we furnish a pseudo-Newtonion potential for accretion disk modeling
around rotating central objects having hard sueface. That means, the potential
may be useful to describe the accretion disk around rotating neutron stars and
strange stars. The potential can describe the general relativistic effects in
accretion disk properly, essentially studying the relativistic hydrodynamics of
disk. As our intention lies in understanding the fluid dynamics of the
accretion disk around rotating central objects with hard surface, it is
necessary to incorporate the rotation of the central object which affects the
inner edge of the disk. We derive our potential, starting from the Hartle
Thorne metric. The potential can reproduce all the essential properties of
general relativity with 10% error at most, for slowly rotating neutron/strange
stars.
