Doenmez, Orhan2019-08-012019-08-0120060218-27181793-6594https://dx.doi.org/10.1142/S0218271806008735https://hdl.handle.net/11480/5505The dynamical evolution of star-disk interaction containing a massive black hole is examined in a region in which physical perturbation dominates other processes and strong gravitational region dominates the potential. The numerical simulation of accretion disk around the black hole is modeled when star is captured by it. When the accretion disk, in steady state or not, is perturbed by the star, the disk around the black hole is destroyed by the star-disk interaction. Destroyed accretion disk creates a spiral shock wave and it causes loss of 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/closedAccessgeneral relativityhydrodynamicsnumerical relativity black holeperturbed accretion diskspiral shockX-rayArticle1571001101510.1142/S02182718060087352-s2.0-33748786528Q2WOS:000241442000003Q2