  We study the solution of viscous accretion disks around rotating
compact/central object having hard surface i.e. neutron star, strange star and
any other highly gravitating objects. We choose pseudo-Newtonian approach to
describe the relativistic accretion disk. For this purpose, the new
pseudo-Newtonian potential is used which is applicable to describe the
relativistic properties of star and its disk. As we know, the Hartle-Thorne
metric can describe geometry of star as well as the space-time out-side of it,
we use this metric for our study. This potential reproduces the marginally
stable orbit exactly as that of general relativity. It also reproduces the
marginally bound orbit and specific mechanical energy at the marginally stable
orbit with at most 4% and 10% error respectively. Using this potential we study
the global parameter space of the accretion disk. Thus, we find out the
physical parameter regime, for which the stable accretion disk can be formed
around gravitating object with hard surface. We show that with the change of
rotation to the central object, the valid disk parameter region dramatically
changes. We also show the effect of viscosity to the fluid properties of the
disk. Subsequently, we give a theoretical prediction of kHz QPO, at least for
one out of a pair, for a fast rotating compact object as 4U 1636-53.
