Numerical Simulation of Rotating Accretion Disk Around the Schwarzschild Black Hole Using GRH Code

Abstract

The 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 consistent with results from Newtonian hydrodynamic code except close to black hole. Newtonian approximation does not give good solution while matter closes to 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 $10M$ and it depends on the specific heat rates. We also find that the smaller $\gamma$ is the more tightly the spiral winds.

arXiv comment19 pages 11 figures

References in corpus (6)

• Three Dimensional Numerical General Relativistic Hydrodynamics I: Formulations, Methods, and Code Tests
• Smoothed Particle Hydrodynamics Confronts Theory: Formation of Standing Shocks in Accretion Disks and Winds Around Black Holes
• Spectral Properties of Accretion Disks Around Black Holes II -- Sub-Keplerian Flows With and Without Shocks
• Smoothed Particle Hydrodynamic Simulations of Viscous Accretion Discs Around Black Holes
• Code Development of Three-Dimensional General Relativistic Hydrodynamics with AMR(Adaptive-Mesh Refinement) and Results From Special and General Relativistic Hydrodynamic
• On the Azimuthal Stability of Shock Waves around Black Holes

Cited by in corpus (2)

• Numerical simulation of small perturbation on an accretion disk due to the collision of a star with the disk near the black hole
• Quasi Periodic Oscillations (QPOs) and frequencies in an accretion disk and comparison with the numerical results from non-rotating black hole computed by the GRH code