مرکز منطقه ای اطلاع رساني علوم و فناوري - Modelling of the Accretion Disk Dynamics Around the Sgr A* Black Hole

Abstract :

The numerical modeling of the disk dynamics around the rotating and non-rotating black holes and revealing the properties of shock wave created on the accretion disk can be achieved by solving the general relativistic hydrodynamic equation using the high resolution shock capturing scheme. It has been observed that the standing shock wave occurred and it is named as tail shock. The tail shock waves are connected to the black hole horizon and the region between two tail shocks are so-called cavity. The properties of shock wave and cavity depend on the adiabatic index of the matter, angular momentum, pressure and black hole rotation parameter. If such shock wave captures the oscillation modes of the disc features, the parameters of the disk and black hole play a important role to determine the properties of the emitted X-rays. The revealing the physical nature of disk oscillation can help to understand the properties of massive black hole which is thought to be located at the center of Sgr A*.