TY - JOUR
T1 - A CHANDRA view of non-thermal emission in the northwestern region of supernova remnant RCW 86
T2 - Particle acceleration and magnetic fields
AU - Castro, Daniel
AU - Lopez, Laura A.
AU - Slane, Patrick O.
AU - Yamaguchi, Hiroya
AU - Ramirez-Ruiz, Enrico
AU - Figueroa-Feliciano, Enectali
N1 - Copyright:
Copyright 2015 Elsevier B.V., All rights reserved.
PY - 2013/12/10
Y1 - 2013/12/10
N2 - The shocks of supernova remnants 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 on board the Chandra X-Ray Observatory, we map and characterize the synchrotron emitting material in the northwest region of RCW 86. We model spectra from several different regions, both filamentary and diffuse, where emission appears to be dominated by synchrotron radiation. The fine spatial resolution of Chandra allows us to obtain accurate emission profiles across three 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 approximately 80 μG.
AB - The shocks of supernova remnants 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 on board the Chandra X-Ray Observatory, we map and characterize the synchrotron emitting material in the northwest region of RCW 86. We model spectra from several different regions, both filamentary and diffuse, where emission appears to be dominated by synchrotron radiation. The fine spatial resolution of Chandra allows us to obtain accurate emission profiles across three 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 approximately 80 μG.
KW - ISM: individual objects (RCW 86)
KW - ISM: supernova remnants
KW - X-rays: ISM
KW - acceleration of particles
KW - cosmic rays
KW - magnetic fields
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U2 - 10.1088/0004-637X/779/1/49
DO - 10.1088/0004-637X/779/1/49
M3 - Article
AN - SCOPUS:84889037594
VL - 779
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 49
ER -