Volume 597, January 2017
|Number of page(s)||18|
|Section||Interstellar and circumstellar matter|
|Published online||13 January 2017|
The connection between supernova remnants and the Galactic magnetic field: An analysis of quasi-parallel and quasi-perpendicular cosmic-ray acceleration for the axisymmetric sample
Dept of Physics and Astronomy, University of Manitoba, Winnipeg, R3T 2N2, Canada
e-mail: firstname.lastname@example.org; email@example.com
Received: 5 January 2016
Accepted: 9 September 2016
The mechanism for the acceleration of cosmic-rays in supernova remnants (SNRs) is an outstanding question in the field. We model a sample of 32 axisymmetric SNRs using the quasi-perpendicular and quasi-parallel cosmic-ray-electron (CRE) acceleration cases. The axisymmetric sample is defined to include SNRs with a double-sided, bilateral morphology, and also those with a one-sided morphology where one limb is much brighter than the other. Using a coordinate transformation technique, we insert a bubble-like model SNR into a model of the Galactic magnetic field. Since radio emission of SNRs is dominated by synchrotron emission and since this emission depends on the magnetic field and CRE distribution, we are able to simulate the SNR emission and compare this to data. We find that the quasi-perpendicular CRE acceleration case is much more consistent with the data than the quasi-parallel CRE acceleration case, with G327.6+14.6 (SN1006) being a notable exception. We propose that SN1006 may be a case where both quasi-parallel and quasi-perpendicular acceleration are simultaneously at play in a single SNR.
Key words: ISM: supernova remnants / ISM: magnetic fields / cosmic rays / radio continuum: ISM / polarization
© ESO, 2017
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