Donmez, O2019-08-012019-08-0120060096-3003https://dx.doi.org/10.1016/j.amc.2005.08.009https://hdl.handle.net/11480/5523The 2D time dependent solution of thin accretion disk in a close binary system have been presented on the equatorial plane around the Schwarzschild black hole. To do that, the special part of the general relativistic hydrodynamical (GRH) equations are solved using high resolution shock capturing (HRSC) schemes. The spiral shock waves on the accretion disk are modeled using perfect fluid equation of state with adiabatic indices gamma = 1.05, 1.2 and 5/3. The results show that the spiral shock waves are created for gammas except the case gamma = 5/3. These results are consistent with the results from Newtonian hydrodynamic code except those which are close to black hole. Newtonian approximation does not give good solution when the matter is close to the black hole. Our simulations illustrate that the spiral shock waves are created close to black hole and the location of inner radius of spiral shock wave is around 6M and it depends on the specific heat rates. We also find that the smaller gamma is the more tightly packed in the spiral winds. (c) 2005 Elsevier Inc. All rights reserved.eninfo:eu-repo/semantics/closedAccessgeneral relativityhydrodynamicsnumerical relativity black holeaccretion diskspiral shockadaptive-mesh refinementArticle175290292210.1016/j.amc.2005.08.0092-s2.0-33645857998Q1WOS:000237568000002Q2