Simulated non-thermal emission from SNR G1.9+0.3

TL;DR

This paper models the non-thermal emission of SNR G1.9+0.3 using 3D magnetohydrodynamic simulations, explaining its ear-shaped morphology and emission features through interaction with a magnetized, asymmetrically shaped circumstellar medium.

Contribution

It introduces a novel 3D simulation approach to explain the morphology and non-thermal emission of SNR G1.9+0.3, linking observed features to the progenitor's stellar wind history.

Findings

Synthetic radio and X-ray maps match observations qualitatively.

The ear-shaped morphology results from interaction with a magnetized, asymmetric circumstellar medium.

Inverse Compton process explains the X-ray emission discrepancies.

Abstract

Supernova remnants are the nebular leftover of defunct stellar environments, resulting from the interaction between a supernova blastwave and the circumstellar medium shaped by the progenitor throughout its life. They display a large variety of non-spherical morphologies such as ears that shine non-thermally. % We have modelled the structure and the non-thermal emission of the supernova remnant G1.9+0.3 through 3D magnetohydrodynamic numerical simulations. We propose that the peculiar ear-shaped morphology of this supernova remnant results from the interaction of the its blast wave with a magnetized circumstellar medium, which was previously asymmetrically shaped by the past stellar wind emanating from the progenitor star or its stellar companion. We created synthetic non-thermal radio and x-ray maps from our simulated remnant structure, which are in qualitative agreement with observations, forming ears on the polar directions. Our synthetic map study explains the discrepancies between the measured non-thermal radio and X-ray surface brightness distributions assuming that the Inverse Compton process produces the observed X-ray emission.