Speaker
Description
We perform general-relativistic magnetohydrodynamic (GRMHD) simulations around the Kerr black hole in a two-temperature paradigm. The goal is to understand the physics around them and extract more accurate physical information from astrophysical observations. Keeping that in mind, we developed a self-consistent numerical formalism to study electron thermodynamics in GRMHD by incorporating heating, radiative cooling, and coupling between electrons and protons. In the talk, I will explain the temperature properties of electrons and ions in the accretion flow around Kerr black holes. We study the role of radiative cooling in both geometrically thick and thin accretion disc scenarios. The temperature profiles of different components show significantly different natures in both physical scenarios. The talk will also explore the inconsistency due to the use of temperature scaling relations and their consequences in near-horizon observations in Sgr A* and M87.
