A Chandra View Of Nonthermal Emission In The Northwestern Region Of Supernova Remnant RCW 86: Particle Acceleration And Magnetic Fields

TL;DR

This study uses Chandra X-ray observations to analyze nonthermal emission in RCW 86, revealing magnetic field amplification and detailed particle acceleration processes in supernova remnant shocks.

Contribution

It provides high-resolution mapping and spectral modeling of synchrotron emission in RCW 86, constraining magnetic field strength and particle acceleration mechanisms.

Findings

Magnetic field strength in filaments is approximately 80 μG.

Narrow filament widths constrain shock acceleration models.

Detailed spectral analysis distinguishes synchrotron emission regions.

Abstract

The shocks of supernova remnants (SNRs) are believed to accelerate particles to cosmic ray (CR) energies. The amplification of the magnetic field due to CRs propagating in the shock region is expected to have an impact on both the emission from the accelerated particle population, as well as the acceleration process itself. Using a 95 ks observation with the Advanced CCD Imaging Spectrometer (ACIS) onboard the Chandra X-ray Observatory, we map and characterize the synchrotron emitting material in the northwestern region of RCW 86. We model spectra from several different regions, filamentary and diffuse alike, where emission appears dominated by synchrotron radiation. The fine spatial resolution of Chandra allows us to obtain accurate emission profiles across 3 different non-thermal rims in this region. The narrow width (l = 10''-30'') of these filaments constrains the minimum magnetic field strength at the post-shock region to be approximately 80 {\mu}G.