Analytical and Monte Carlo results for the surface-brightness diameter relationship in supernova remnants

TL;DR

This paper models the surface brightness-diameter relationship in supernova remnants using analytical and Monte Carlo methods, introducing new models and a novel density distribution function to explain observed fluctuations.

Contribution

It presents a combined analytical and Monte Carlo approach with new density modeling to better understand supernova remnants' surface brightness evolution.

Findings

Monte Carlo simulations replicate observed fluctuations.

New density distribution function improves model accuracy.

Analytical models align with observational data.

Abstract

The surface brightness diameter relationship for supernovae remnants (SNRs) is explained by adopting a model of direct conversion of the flux of kinetic energy into synchrotron luminosity. Two laws of motion are adopted, a power law model for the radius-time relationship, and a model which uses the thin layer approximation. The fluctuations on the log-log surface diameter relationship are modeled by a Monte Carlo simulation. In this model a new probability density function for the density as function of the galactic height is introduced.