3D MHD simulations of the supernova remnant CTB 109

TL;DR

This study uses 3D MHD simulations to model the evolution and emission of supernova remnant CTB 109, revealing conditions for its formation and explaining observed magnetic field and emission features.

Contribution

First 3D MHD simulations of CTB 109 that incorporate a two-medium environment and magnetic field effects to explain its observed properties.

Findings

Remnant forms if SN occurs in less dense medium with uniform magnetic field.

Quasiparallel mechanism explains synchrotron brightness and magnetic field orientation.

Remnant evolution consistent with observed features of CTB 109.

Abstract

We examine the evolution and emission of the supernova remnant (SNR) CTB109 using three-dimensional magnetohydrodynamics simulations. The SNR evolves in a medium divided by a plane interface into two media with different densities and pressure equilibrium. Our results reveal that a remnant with the characteristics of CTB109 is formed provided the supernova (SN) explosion takes place in the less dense medium and also if the interstellar magnetic field (ISMF) is almost uniform. Finally, we conclude that the quasiparallel mechanism can explain the brightness synchrotron emission and the position angle of the projected ISMF reported in previous works.