MC Simulations of the Broadband Spectra of Sagittarius A* through the use of GRMHD

TL;DR

This paper combines GRMHD and Monte Carlo simulations to model Sagittarius A*'s broadband spectrum, fitting observational data across radio, IR, and X-ray wavelengths.

Contribution

It introduces a coupled GRMHD and Monte Carlo simulation approach to accurately model the accretion flow spectrum of Sagittarius A*.

Findings

Successfully fits radio, IR, and X-ray observational data.

Assesses the scaling of physical parameters needed for the model.

Provides insights into the physical conditions near Sagittarius A*.

Abstract

We present results of simulations of the spectrum of the accretion flow onto the supermassive black hole in our Galactic Centre, Sagittarius A*, generated with a coupling of Monte-Carlo (MC) radiation and general relativistic magnetohydrodynamic (GRMHD) codes. In our modeling, we use the 2D HARM GRMHD code to first model the physical parameters of the disk, then feed its results into our 2D MC photon transport code. We will discuss results obtained which fit radio, IR, and Chandra-obtained flaring or quiescent x-ray data points, as well as the validity of the amount of scaling of input parameters (density, temperature, and magnetic field) required to fit these points. HARM output will be used to suggest whether the scaling is within reasonable limits.