Doenmez, O.Cetin, SAHikmet, I2019-08-012019-08-012007978-0-7354-0404-50094-243Xhttps://hdl.handle.net/11480/54526th International Conference of the Balkan-Physical-Union -- AUG 22-26, 2006 -- Istanbul, TURKEYIn this paper, perturbations of an accretion disk by a star orbiting around a massive black hole are studied. We report on a numerical experiment, which has been carried out by using a parallel-machine code originally developed by Ref.[1]. An initially steady state accretion disk near a non-rotating (Schwarzschild) black hole interacts with a "star", modeled as an initially circular region of increased density. Part of the disk is affected by the interaction. We follow the evolution for order of one dynamical period and we show how the non-axisymetric density perturbation further evolves and moves downward where the material of the disk and the star become eventually accreted onto the central body. When the accretion disk, in steady state or not, is perturbed by star, disk around the black hole is destroyed by the star-disk interaction. Destroyed accretion disks at different locations create spiral shock waves and they causes losing its angular momentum. Finally, because of losing angular momentum, gas starts falling into the black hole. At the same time, X-ray is emitted by accretion disk during the unstable cases. The massive black hole may be created as a consequence of interaction.eninfo:eu-repo/semantics/closedAccessrelativistic hydrodynamicsaccretion diskstar-disk interactionAGNshock waveConference Object8991431442-s2.0-34547488468N/AWOS:000246647900050N/A