New perspectives on the supernova remnant Puppis A based on a radio polarization study

TL;DR

This study uses radio polarization observations to analyze the magnetic field structure and morphology of supernova remnant Puppis A, revealing a low polarization fraction and magnetic alignment consistent with evolution inside a stellar wind bubble.

Contribution

It provides new insights into Puppis A's magnetic field configuration and morphology, supporting a stellar wind bubble evolution scenario over previous density gradient models.

Findings

Low polarization fraction (~3%) observed.

Magnetic vectors show two preferential directions aligned with the shell edges.

Evidence of magnetic field alignment with shock front direction.

Abstract

We present a polarization study towards the supernova remnant (SNR) Puppis A based on original observations performed with the Australia Telescope Compact Array (ATCA). Based on the analysis of a feature detected outside the SNR shell (called `the tail' throughout the paper), it was possible to disentangle the emission with origin in Puppis A itself from that coming from the foreground Vela SNR. We found a very low polarization fraction, of about 3 percent on average. The upper limit of the magnetic field component parallel to the line of sight is estimated to be B$_\parallel \sim$ 20 $\mu$G. The statistical behavior of the magnetic vectors shows two preferential directions, almost perpendicular to each other, which are approximately aligned with the flat edges of Puppis A. A third, narrow peak oriented perpendicular to the Galactic plane suggests the existence of an interstellar magnetic field locally aligned in this direction. There is evidence that the magnetic vectors along the shell are aligned with the shock front direction. The low polarization fraction and the statistical behavior of the magnetic vectors are compatible with a scenario where the SNR evolves inside a stellar wind bubble with a box-like morphology, produced by the interaction of the different stellar winds, one of them magnetized, launched by the SN progenitor. This scenario can furthermore explain the morphology of Puppis A, rendering little support to the previously accepted picture which involved strong density gradients to explain the flat, eastern edge of the shell.