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

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 μG.

7 pages, 3 figures, submitted for publication at the Astrophysical Journal

References in corpus (4)

• Observational constraints on energetic particle diffusion in young SNRs: amplified magnetic field and maximum energy
• Measuring the cosmic ray acceleration efficiency of a supernova remnant
• Nonlinear Diffusive Shock Acceleration with Magnetic Field Amplification
• Proper Motions of H-alpha filaments in the Supernova Remnant RCW 86

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