Speaker
Description
The matter orbiting black hole (BH) in micro-quasar or active galactic nuclei forms toroidal accretion disk structures, and multiple tori structures have been recently described as ringed accretion disks (RADs) in full general relativistic approach. We realize a full general relativistic magnetohydrodynamic (GRMHD) numerical simulations related to double toroidal structure immersed into the equatorial plane of gravitomagnetic field of central Schwarzschild BH in an asymptotically uniform magnetic field. We study the collisional dynamic of an initial RAD structure constructed by two co-rotating or counter-rotating tori, where the accretion of matter from the outer torus is assumed onto the inner torus, using the 2.5D GRMHD simulation schemes with HARM numerical code. We study the dynamics of the system assuming various initial conditions and we have demonstrated that initial matter density is the relevant factor governing the system evolution.
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