Ion injection and acceleration at modified shocks
| dc.creator | Gieseler, U. D. J. | |
| dc.creator | Jones, T. W. | |
| dc.creator | Kang, Hyesung | |
| dc.date | 1999-06-07 | |
| dc.date.accessioned | 2026-07-07T02:31:52Z | |
| dc.date.available | 2026-07-07T02:31:52Z | |
| dc.description | The theory of diffusive particle acceleration explains the spectral properties of the cosmic rays below energies of approx. 10^6 GeV as produced at strong shocks in supernova remnants (SNR's). To supply the observed flux of cosmic rays, a significant fraction of the energy released by a supernova has to be transfered to cosmic rays. The key to the question of the efficiency of SNR's in producing cosmic rays is the injection process from thermal energies. A self-consistent model has to take into account the interaction of the accelerated particles with magneto-hydrodynamic waves, which generate the particle diffusion, a requisite for the acceleration process. Such a nonlinear model of the turbulent background plasma has been developed recently (Malkov, 1998, Phys. Rev. E 58, 4911). We use this model for the first numerical treatment of the gas dynamics and the diffusion-convection equation at a quasi-parallel strong shock, which incorporates a plasma-physical injection model to investigate the cosmic ray production. | |
| dc.description | 4 pages, to be published in the Proceedings of the 26th ICRC, Salt Lake City, 1999, OG 3.3.20 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9906114 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9906114 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/14312 | |
| dc.subject | Astrophysics | |
| dc.title | Ion injection and acceleration at modified shocks | |
| dc.type | text |