  The mechanism for 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 SNRs 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.
