# Magnetic Reconnection Detonation in Supernova Remnants

## Author(s): Zhang, H; Gao, Y; Law, Chung K

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DC FieldValueLanguage
dc.contributor.authorZhang, H-
dc.contributor.authorGao, Y-
dc.contributor.authorLaw, Chung K-
dc.date.accessioned2021-10-08T20:19:50Z-
dc.date.available2021-10-08T20:19:50Z-
dc.date.issued2018en_US
dc.identifier.citationZhang, H, Gao, Y, Law, CK. (2018). Magnetic Reconnection Detonation in Supernova Remnants. Astrophysical Journal, 864 (10.3847/1538-4357/aad819en_US
dc.identifier.urihttp://arks.princeton.edu/ark:/88435/pr17c6s-
dc.description.abstractExpansion of supernova remnants (SNRs) is a key process that refreshes the interstellar medium (ISM) in which a new generation of stars is born. The dynamics and radiative properties of the SNR expansion front not only reflect the physical environment of the old ISM surrounding the supernova, but they also provide information about the refreshed ISM. However there are challenges arising from recent observations: the expansion of SNRs cannot be simply explained by the conventional law of shock wave expansion, while the high energy radiation requires an additional electron acceleration mechanism in the shock front beyond thermal collision. We consider herein the detonation wave description of the SNR expansion, in which magnetic reconnection follows the shock front and transfers the magnetic field energy to both the fluid thermal energy and particle kinetic energy. The structure of the magnetic reconnection detonation (MRD) model is identified based on scaling analysis, in which properties of both the old and refreshed ISM are also predicted.en_US
dc.language.isoen_USen_US
dc.relation.ispartofAstrophysical Journalen_US
dc.rightsAuthor's manuscripten_US
dc.titleMagnetic Reconnection Detonation in Supernova Remnantsen_US
dc.typeJournal Articleen_US