3D MHD simulation of polarized emission in SN 1006

TL;DR

This study uses 3D MHD simulations to model polarized emission in SN 1006, comparing two particle acceleration mechanisms and supporting the quasi-parallel model through synthetic and observational map analysis.

Contribution

It introduces a polarization simulation approach to distinguish particle acceleration mechanisms in supernova remnants, favoring the quasi-parallel model for SN 1006.

Findings

Synthetic polarization maps match observations best with the quasi-parallel mechanism.

The study provides a new method to identify acceleration mechanisms in supernova remnants.

Supports the quasi-parallel model as the dominant acceleration process in SN 1006.

Abstract

We use three dimensional magnetohydrodynamic (MHD) simulations to model the supernova remnant SN 1006. From our numerical results, we have carried out a polarization study, obtaining synthetic maps of the polarized intensity, the Stokes parameter $Q$, and the polar-referenced angle, which can be compared with observational results. Synthetic maps were computed considering two possible particle acceleration mechanisms: quasi-parallel and quasi-perpendicular. The comparison of synthetic maps of the Stokes parameter $Q$ maps with observations proves to be a valuable tool to discern unambiguously which mechanism is taking place in the remnant of SN 1006, giving strong support to the quasi-parallel model.