Numerical simulation of the disk dynamics around the black hole: Bondi–Hoyle accretion

摘要: We have solved the General Relativistic Hydrodynamic (GRH) equations using high resolution shock capturing scheme (HRSCS) to find out dependency of disk dynamics Mach number, adiabatic index, black hole rotation parameter and outer boundary computational domain around non-rotating rotating holes. inject gas at upstream downstream regions same time with different initial conditions. It is found that variety mass accretion rates cone structures strongly depend on number index gas. The cones are important physical mechanisms trap existing oscillation modes, thereupon these trapped modes may generate strong X-rays observed by X-ray satellites. Besides, our numerical approach also show produces flip–flop instabilities which monitored in simulations explain erratic spin behavior compact objects (the holes neutron stars) seen from data.