On the effect of the pulsar magnetodipole radiation on the supernova remnant

Details On the effect of the pulsar magnetodipole radiation on the supernova remnant On the effect of the pulsar magnetodipole radiation on the supernova remnant

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.306..191l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 306, Issue 1, pp. 191-198.

Astronomy and Astrophysics

Astronomy

6

Hydrodynamics, Methods: Numerical, Pulsars: General, Supernova Remnants

Scientific paper

The interaction between a pulsar and a supernova remnant, both originating in the same Type II supernova explosion, is presented. It is assumed that the magnetodipole radiation emitted by the pulsar cannot penetrate the remnant material, and a low-frequency radiation-filled cavity thus forms surrounding the pulsar. This effect has been modelled by first considering the evolution of the blast wave in the progenitor star, with an idealized density distribution of the form rho ~ r^-2 surrounded by a uniform circumstellar environment, until radiation pressure within the remnant material becomes negligible as a result of expansion. Assuming then that the remnant material expands ballistically, the effect of the pulsar-induced cavity is to power the expansion of a thin shell of material which, depending on the initial spin frequency of the pulsar, can sweep through the ejecta and eventually reach the blast wave. Results for the evolution of density, velocity, pressure and radius of the thin shell are presented. It is shown here that, for a pulsar born with the maximum possible spin frequency, the cavity shell will strike the frontmost part of the shocked gas ~ 60 yr after the supernova explosion. Such pulsar-supernova remnant interactions are proposed to form the base of a subclassification of pulsar-filled supernova remnants.

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