Supernova Remnant and Pulsar Wind Nebula Interactions

Details Supernova Remnant and Pulsar Wind Nebula Interactions Supernova Remnant and Pulsar Wind Nebula Interactions

2003-10-16

arxiv.org/abs/astro-ph/0310471v1

Astronomy and Astrophysics

Astrophysics

8 pages, review, for "3-D Signatures in Stellar Explosions: A Workshop honoring J. Craig Wheeler's 60th birthday," held June 1

Scientific paper

I review several topics in the structure of supernova remnants. Hydrodynamic instabilities in young remnants may give rise to the cellular structure that is sometimes observed, although structure in the ejecta might also play a role. The presence of ejecta close to the forward shock front of a young remnant can be the result of ejecta clumps or the dynamical effects of cosmic rays. Slower moving ejecta clumps can affect the outer shock structure of older remnants such as Vela. Young remnants typically show a circular structure, but often have a one-sided asymmetry; the likely reasons are an asymmetric circumstellar medium, or pulsar velocities in the case of pulsar wind nebulae. In older remnants, asymmetric pulsar wind nebulae can result from asymmetric reverse shock flows and/or pulsar velocities.

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