Time-Dependent Models for a decade of SN 1993J

TL;DR

This paper develops classical and relativistic models for supernova remnant expansion, incorporating interstellar medium density profiles and relativistic hydrodynamics, and validates these models against ten years of SN 1993J observations.

Contribution

It introduces new relativistic equations of motion with pressure for supernova remnants and calibrates them using extensive observational data.

Findings

Models accurately fit ten years of SN 1993J data.

Relativistic hydrodynamics with pressure explains intensity profiles.

Inverse power law density assumptions improve model precision.

Abstract

A classical and a relativistic law of motion for a supernova remnant (SNR) are deduced assuming an inverse power law behavior for the density of the interstellar medium and applying the thin layer approximation. A third equation of motion is found in the framework of relativistic hydrodynamics with pressure, applying momentum conservation. These new formulas are calibrated against a decade of observations of \snr. The existing knowledge of the diffusive processes of ultrarelativistic electrons is reviewed in order to explain the behavior of the `U' shaped profile of intensity versus distance from the center of SN 1993J.