Non-thermal radio supernova remnants of exiled Wolf-Rayet stars

TL;DR

This study uses 2D magneto-hydrodynamical simulations to explore how interstellar magnetic fields influence the shape and radio emission of supernova remnants from exiled Wolf-Rayet stars, revealing magnetic effects on remnant morphology.

Contribution

It demonstrates the impact of ambient magnetic fields on the morphology and radio features of supernova remnants from high-velocity Wolf-Rayet stars, a novel focus in remnant modeling.

Findings

Magnetic fields modify shock front properties and suppress filament formation.

Magnetic compression stabilizes wind/ISM contact discontinuity.

Simulated radio features match observed remnants like G296.5+10.0, CTB109, and Kes 17.

Abstract

A signification fraction of Galactic massive stars (> 8Mo) are ejected from their parent cluster and supersonically sail away through the interstellar medium (ISM). The winds of these fast-moving stars blow asymmetric bubbles thus creating a circumstellar environment in which stars eventually die with a supernova explosion. The morphology of the resulting remnant is largely governed by the circumstellar medium of the defunct progenitor star. In this paper, we present 2D magneto-hydrodynamical simulations investigating the effect of the ISM magnetic field on the shape of the supernova remnants of a 35Mo star evolving through a Wolf-Rayet phase and running with velocity 20 and 40 km/s, respectively. A 7 microG ambient magnetic field is sufficient to modify the properties of the expanding supernova shock front and in particular to prevent the formation of filamentary structures. Prior to the supernova explosion, the compressed magnetic field in the circumstellar medium stabilises the wind/ISM contact discontinuity in the tail of the wind bubble. A consequence is a reduced mixing efficiency of ejecta and wind materials in the inner region of the remnant, where the supernova shock wave propagates. Radiative transfer calculations for synchrotron emission reveal that the non-thermal radio emission has characteristic features reflecting the asymmetry of exiled core-collapse supernova remnants from Wolf-Rayet progenitors. Our models are qualitatively consistent with the radio appearance of several remnants of high-mass progenitors, namely the bilateral G296.5+10.0 and the shell-type remnants CTB109 and Kes 17, respectively.