Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 849, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/2041-8213/aa94c4
Keywords
cosmic rays; ISM: magnetic fields; ISM: supernova remnants; polarization; radio continuum: ISM
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Funding
- University of Toronto
- Natural Sciences and Engineering Research Council of Canada (NSERC) [RGPIN-2015-05948]
- Canada Research Chairs program
- NSERC
- CSA
- CFI
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Radial magnetic fields are observed in all known young, shell-type supernova remnants in our Galaxy, including Cas A, Tycho, Kepler, and SN1006, and yet the nature of these radial fields has not been thoroughly explored. Using a 3D model, we consider the existence and observational implications of an intrinsically radial field. We also present a new explanation of the origin of the radial pattern observed from polarization data as resulting from a selection effect due to the distribution of cosmic-ray electrons (CREs). We show that quasi-parallel acceleration can concentrate CREs at regions where the magnetic field is radial, making a completely turbulent field appear ordered, when it is in fact disordered. We discuss observational properties that may help distinguish between an intrinsically radial magnetic field and the case where it only appears radial due to the CRE distribution. We also show that the case of an intrinsically radial field with a quasi-perpendicular CRE acceleration mechanism has intriguing similarities to the observed polarization properties of SN1006.
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