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

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