A Monte Carlo Code for Relativistic Radiation Transport Around Kerr Black Holes

TL;DR

This paper introduces a new Monte Carlo simulation code for relativistic radiation transport near Kerr black holes, capable of handling complex emission, absorption, scattering, and polarization effects in accretion flows.

Contribution

The paper presents a novel Monte Carlo code that models relativistic radiation transport around Kerr black holes with comprehensive physical processes included.

Findings

Code accurately models radiation transport in Kerr spacetime

Numerical tests demonstrate good convergence and reliability

Applicable to studying accretion disk and corona emissions

Abstract

We present a new code for radiation transport around Kerr black holes, including arbitrary emission and absorption terms, as well as electron scattering and polarization. The code is particularly useful for analyzing accretion flows made up of optically thick disks and optically thin coronae. We give a detailed description of the methods employed in the code, and also present results from a number of numerical tests to assess its accuracy and convergence.