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

Abstract

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.

22 pages, 6 figures

References in corpus (9)

• Radio observational constraints on Galactic 3D-emission models
• The Youngest Galactic Supernova Remnant: G1.9+0.3
• First detection of VHE gamma-rays from SN 1006 by H.E.S.S
• Simulating polarized Galactic synchrotron emission at all frequencies, the Hammurabi code
• On the Origin of Asymmetries in Bilateral Supernova Remnants
• The radio expansion and brightening of the very young supernova remnant G1.9+0.3
• Aspect angle for interstellar magnetic field in SN 1006
• 3D MHD simulation of polarized emission in SN 1006
• The radio SNR G65.1+0.6 and its associated pulsar J1957+2831

Cited by in corpus (5)

• Mysterious Odd Radio Circle near the Large Magellanic Cloud -- An Intergalactic Supernova Remnant?
• When disorder looks like order: a new model to explain radial magnetic fields in young supernova remnants
• Quasi-perpendicular shock acceleration and TDE radio flares
• Electron Energization in Quasi-Parallel Shocks: Test-Particle-Electrons in a Proton Driven Turbulence
• On the Potential of Faraday Tomography to Identify Shock Structures in Supernova Remnants