Volume 380, Number 1, December II 2001
|Page(s)||309 - 317|
|Published online||15 December 2001|
Pulsar wind nebulae in supernova remnants
Spherically symmetric hydrodynamical simulations
Astronomical Institute, Utrecht University, PO Box 80000, 3508 TA Utrecht, The Netherlands
2 Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Republic of Ireland
3 Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
4 Service d'Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France
5 Department of Atomic Physics, Pázmány Péter sétány 1, 1117 Budapest, Hungary
Corresponding author: E. van der Swaluw, firstname.lastname@example.org
Accepted: 27 September 2001
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.
Key words: ISM: supernova remnants / stars: pulsars: general / hydrodynamics / shock waves
© ESO, 2001
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