Abstract
A few important astronomical phenomena are powered by supermassive black holes undergoing super-Eddington accretion, such as tidal disruption events, narrow line Seyfert 1 galaxies and, most important, luminous quasars recently detected at high redshifts. In this talk, I will describe my work on using state-of-the-art global three-dimensional general relativistic radiation magnetohydrodynamical (GRRMHD) simulations to study gas flows undergoing super-Eddington accretion around supermassive black holes and analysing their energetic outputs. In particular, I focus on studying how the outflow mechanical energy and emission radiation energy depend on the gas accretion rate around both spinning and non-spinning black holes. I also compare my results with recent observations and discuss the applications of my simulation results in future cosmological simulations.
Anyone interested is welcome to attend.