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In this paper, perturbations of an accretion disk by a star orbiting around ablack hole are studied. We report on a numerical experiment, which has beencarried out by using a parallel-machine code originally developed by D\"{o}nmez(2004). An initially steady state accretion disk near a non-rotating(Schwarzschild) black hole interacts with a "star", modeled as an initiallycircular region of increased density. Part of the disk is affected by theinteraction. In some cases, a gap develops and shock wave propagates throughthe disk. We follow the evolution for order of one dynamical period and we showhow the non-axisymetric density perturbation further evolves and movesdownwards where the material of the disk and the star become eventuallyaccreted onto the central body.  When the star perturbs the steady state accretion disk, the disk around theblack hole is destroyed by the effect of perturbation. The perturbed accretiondisk creates a shock wave during the evolution and it loses angular momentumwhen the gas hits on the shock waves. Colliding gas with the shock wave is theone of the basic mechanism of emitting the $X-$rays in the accretion disk. Theseries of supernovae occurring in the inner disk could entirely destroy thedisk in that region which leaves a more massive black hole behind, at thecenter of galaxies.Comment: 20pages, 8 figures, accepted for publication in Astrophysics and  Space Scienc

Numerical Simulation of Small Perturbation on an Accretion Disk Due to the Collision of a Star with the Disk Near the Black Hole