Cosmic ray acceleration in young supernova remnants
We investigate the appearance of magnetic field amplification resulting from a cosmic ray escape current in the context of supernova remnant shock waves. The current is inversely proportional to the maximum energy of cosmic rays, and is a strong function of the shock velocity. Depending on the evolu...
| Main Authors: | , |
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| Format: | Journal article |
| Language: | English |
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2013
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| _version_ | 1797092133964873728 |
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| author | Schure, K Bell, A |
| author_facet | Schure, K Bell, A |
| author_sort | Schure, K |
| collection | OXFORD |
| description | We investigate the appearance of magnetic field amplification resulting from a cosmic ray escape current in the context of supernova remnant shock waves. The current is inversely proportional to the maximum energy of cosmic rays, and is a strong function of the shock velocity. Depending on the evolution of the shock wave, which is drastically different for different circumstellar environments, the maximum energy of cosmic rays as required to generate enough current to trigger the non-resonant hybrid instability that confines the cosmic rays follows a different evolution and reaches different values.We find that the best candidates to accelerate cosmic rays to ~ few PeV energies are young remnants in a dense environment, such as a red supergiant wind, as may be applicable to Cassiopeia A. We also find that for a typical background magnetic field strength of 5 μG the instability is quenched in about 1000 years, making SN1006 just at the border of candidates for cosmic ray acceleration to high energies. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. |
| first_indexed | 2024-03-07T03:41:56Z |
| format | Journal article |
| id | oxford-uuid:be32ff6e-40e5-49a6-825b-e89bc75dce31 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T03:41:56Z |
| publishDate | 2013 |
| record_format | dspace |
| spelling | oxford-uuid:be32ff6e-40e5-49a6-825b-e89bc75dce312022-03-27T05:37:25ZCosmic ray acceleration in young supernova remnantsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:be32ff6e-40e5-49a6-825b-e89bc75dce31EnglishSymplectic Elements at Oxford2013Schure, KBell, AWe investigate the appearance of magnetic field amplification resulting from a cosmic ray escape current in the context of supernova remnant shock waves. The current is inversely proportional to the maximum energy of cosmic rays, and is a strong function of the shock velocity. Depending on the evolution of the shock wave, which is drastically different for different circumstellar environments, the maximum energy of cosmic rays as required to generate enough current to trigger the non-resonant hybrid instability that confines the cosmic rays follows a different evolution and reaches different values.We find that the best candidates to accelerate cosmic rays to ~ few PeV energies are young remnants in a dense environment, such as a red supergiant wind, as may be applicable to Cassiopeia A. We also find that for a typical background magnetic field strength of 5 μG the instability is quenched in about 1000 years, making SN1006 just at the border of candidates for cosmic ray acceleration to high energies. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. |
| spellingShingle | Schure, K Bell, A Cosmic ray acceleration in young supernova remnants |
| title | Cosmic ray acceleration in young supernova remnants |
| title_full | Cosmic ray acceleration in young supernova remnants |
| title_fullStr | Cosmic ray acceleration in young supernova remnants |
| title_full_unstemmed | Cosmic ray acceleration in young supernova remnants |
| title_short | Cosmic ray acceleration in young supernova remnants |
| title_sort | cosmic ray acceleration in young supernova remnants |
| work_keys_str_mv | AT schurek cosmicrayaccelerationinyoungsupernovaremnants AT bella cosmicrayaccelerationinyoungsupernovaremnants |