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The mechanism for acceleration of cosmic rays in supernova remnants (SNRs) isan outstanding question in the field. We model a sample of 32 axisymmetric SNRsusing the quasi-perpendicular and quasi-parallel cosmic-ray-electron (CRE)acceleration cases. The axisymmetric sample is defined to include SNRs with adouble-sided, bilateral morphology, and also those with a one-sided morphologywhere one limb is much brighter than the other. Using a coordinatetransformation technique, we insert a bubble-like model SNR into a model of theGalactic magnetic field. Since radio emission of SNRs is dominated bysynchrotron emission and since this emission depends on the magnetic field andCRE distribution, we are able to simulate the SNRs emission and compare this todata. We find that the quasi-perpendicular CRE acceleration case is much moreconsistent with the data than the quasi-parallel CRE acceleration case, withG327.6+14.6 (SN1006) being a notable exception. We propose that SN1006 may be acase where both quasi-parallel and quasi-perpendicular acceleration aresimultaneously at play in a single SNR.

astronomy and astrophysics

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