A Model for the X-Ray Luminosity of Pulsar Nebulae

Details A Model for the X-Ray Luminosity of Pulsar Nebulae A Model for the X-Ray Luminosity of Pulsar Nebulae

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...539l..45c&link_type=abstract

The Astrophysical Journal, Volume 539, Issue 1, pp. L45-L48.

Astronomy and Astrophysics

Astronomy

64

Stars: Pulsars: General, Shock Waves, Ism: Supernova Remnants, X-Rays: General

Scientific paper

A one-zone, shocked wind model is developed for the X-ray luminosity of pulsar nebulae. If the electrons and positrons cool rapidly by synchrotron radiation and the initial particle spectrum is similar to that of the Crab Nebula, the X-ray luminosity is produced from the pulsar power with high efficiency and is insensitive to the model parameters. If the electrons are not in the cooling regime, the X-ray luminosity is produced with lower efficiency, as appears to be the case for the compact nebula around the Vela pulsar. The observed X-ray spectral index is an indicator for which case applies and thus plays a role in estimating the pulsar power needed to produce an observed X-ray luminosity.

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