Origin of the bilateral structure of the supernova remnant G296.5+10

TL;DR

This paper models the supernova remnant G296.5+10 using 3D MHD simulations to explain its bilateral shape and magnetic features, highlighting the role of progenitor and Galactic magnetic fields in its morphology.

Contribution

It introduces a comprehensive 3D MHD model that accounts for the remnant's morphology and magnetic properties, including polarization and rotation measure differences.

Findings

The remnant's morphology is explained by expansion into a magnetic field shaped by the progenitor and Galactic fields.

The polarization maps support the quasi-parallel acceleration mechanism at the shock front.

Differences in rotation measure are consistent with the combined magnetic field model.

Abstract

In the present work we have modeled the supernova remnant (SNR) G296.5+10, by means of 3D magnetohydrodynamics (MHD) simulations. This remnant belongs to the bilateral SNR group and has an additional striking feature: the rotation measure (RM) in its eastern and western parts are very different. In order to explain both the morphology observed in radio-continuum and the RM, we consider that the remnant expands into a medium shaped by the superposition of the magnetic field of the progenitor star with a constant Galactic magnetic field. We have also carried out a polarization study from our MHD results, obtaining synthetic maps of the linearly polarized intensity and the Stokes parameters. This study reveals that both the radio morphology and the reported RM for G$296.5+10$ can be explained if the quasi-parallel acceleration mechanism is taking place in the shock front of this remnant.