Interaction of a magnetized pulsar wind with its surroundings. MHD simulations of Pulsar Wind Nebulae

Abstract

Magnetohydrodynamical simulations are presented of a magnetized pulsar wind interacting directly with the interstellar medium, or, in the case of a surrounding supernova remnant, with the associated freely expanding ejecta of the progenitor star. In both cases the simulations show that the pulsar wind nebula will be elongated due to the dynamical influence of the toroidal magnetic fields, which confirm predictions from a semi-analytical model presented by Begelman & Li. The simulations follow the expansion of the pulsar wind nebula when the latter is bounded by a strong shock and show that the expansion can be modeled with a standard power-law expansion rate. By performing different simulations with different magnetization parameters, I show that the latter weakly correlates with the elongation of the pulsar wind nebula. The results from the simulations are applied to determine the nature of the expansion rate of the pulsar wind nebula 3C58. It is shown that there is both observational and theoretical evidence which supports the scenario in which the pulsar wind nebula 3C58 has caught up with the reverse shock of the associated (but undetected) supernova remnant.

9 pages, 8 figures, accepted for A&A

References in corpus (6)

• Pulsar Wind Nebulae in Evolved Supernova Remnants
• Discovery of X-ray Pulsations from the Compact Central Source in the Supernova Remnant 3C 58
• Interaction of High-Velocity Pulsars with Supernova Remnant Shells
• Towards Resolving the Crab $\sigma -$Problem: A Linear Accelerator?
• Radio Spectral Index and Expansion of 3C58
• Spectral Components of the Radio Composite Supernova Remnant G11.2-0.3

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