Pulsar wind nebulae in supernova remnants
| dc.creator | van der Swaluw, E. | |
| dc.creator | Achterberg, A. | |
| dc.creator | Gallant, Y. A. | |
| dc.creator | Tóth, G. | |
| dc.date | 2000-12-20 | |
| dc.date.accessioned | 2026-07-07T01:57:07Z | |
| dc.date.available | 2026-07-07T01:57:07Z | |
| dc.description | A spherically symmetric model is presented for the interaction of a pulsar wind with the associated supernova remnant. This results in a pulsar wind nebula whose evolution is coupled to the evolution of the surrounding supernova remnant. This evolution can be divided in three stages. The first stage is characterised by a supersonic expansion of the pulsar wind nebula into the freely expanding ejecta of the progenitor star. In the next stage the pulsar wind nebula is not steady; the pulsar wind nebula oscillates between contraction and expansion due to interaction with the reverse shock of the supernova remnant: reverberations which propagate forward and backward in the remnant. After the reverberations of the reverse shock have almost completely vanished and the supernova remnant has relaxed to a Sedov solution, the expansion of the pulsar wind nebula proceeds subsonically. In this paper we present results from hydrodynamical simulations of a pulsar wind nebula through all these stages in its evolution. The simulations were carried out with the Versatile Advection Code. | |
| dc.description | 10 pages, 9 figures, submitted to Astronomy and Astrophysics | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0012440 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0012440 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/2260 | |
| dc.subject | Astrophysics | |
| dc.title | Pulsar wind nebulae in supernova remnants | |
| dc.type | text |