Magnetic field amplification by cosmic rays in supernova remnants
Magnetic field amplification is needed to accelerate cosmic cays to PeV energies in supernova remants. Escaping cosmic rays trigger a return current in the plasma that drives a non-resonant hybrid instability. We run simulations in which we represent the escaping cosmic rays with the plasma return c...
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| Format: | Conference item |
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2012
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| _version_ | 1797062897488101376 |
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| author | Schure, K Bell, A |
| author_facet | Schure, K Bell, A |
| author_sort | Schure, K |
| collection | OXFORD |
| description | Magnetic field amplification is needed to accelerate cosmic cays to PeV energies in supernova remants. Escaping cosmic rays trigger a return current in the plasma that drives a non-resonant hybrid instability. We run simulations in which we represent the escaping cosmic rays with the plasma return current, keeping the maximum cosmic ray energy fixed, and evaluate its effects on the upstream medium. In addition to magnetic field amplification, density perturbations arise that, when passing through the shock, further increase amplification levels downstream. As the growth rate of the instability is most rapid for the smaller scales, the resolution is a limiting factor in the amplification that can be reached with these simulations. |
| first_indexed | 2024-03-06T20:52:07Z |
| format | Conference item |
| id | oxford-uuid:37f120fb-22b0-4e70-9460-44e612fdd877 |
| institution | University of Oxford |
| last_indexed | 2024-03-06T20:52:07Z |
| publishDate | 2012 |
| record_format | dspace |
| spelling | oxford-uuid:37f120fb-22b0-4e70-9460-44e612fdd8772022-03-26T13:46:58ZMagnetic field amplification by cosmic rays in supernova remnantsConference itemhttp://purl.org/coar/resource_type/c_5794uuid:37f120fb-22b0-4e70-9460-44e612fdd877Symplectic Elements at Oxford2012Schure, KBell, AMagnetic field amplification is needed to accelerate cosmic cays to PeV energies in supernova remants. Escaping cosmic rays trigger a return current in the plasma that drives a non-resonant hybrid instability. We run simulations in which we represent the escaping cosmic rays with the plasma return current, keeping the maximum cosmic ray energy fixed, and evaluate its effects on the upstream medium. In addition to magnetic field amplification, density perturbations arise that, when passing through the shock, further increase amplification levels downstream. As the growth rate of the instability is most rapid for the smaller scales, the resolution is a limiting factor in the amplification that can be reached with these simulations. |
| spellingShingle | Schure, K Bell, A Magnetic field amplification by cosmic rays in supernova remnants |
| title | Magnetic field amplification by cosmic rays in supernova remnants |
| title_full | Magnetic field amplification by cosmic rays in supernova remnants |
| title_fullStr | Magnetic field amplification by cosmic rays in supernova remnants |
| title_full_unstemmed | Magnetic field amplification by cosmic rays in supernova remnants |
| title_short | Magnetic field amplification by cosmic rays in supernova remnants |
| title_sort | magnetic field amplification by cosmic rays in supernova remnants |
| work_keys_str_mv | AT schurek magneticfieldamplificationbycosmicraysinsupernovaremnants AT bella magneticfieldamplificationbycosmicraysinsupernovaremnants |