A model for the X-ray luminosity of pulsar nebulae

被引：69

作者：

Chevalier, RA ^{[1
]}

机构：

[1] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA

来源：

ASTROPHYSICAL JOURNAL | 2000年 / 539卷 / 01期

基金：

美国国家航空航天局;

关键词：

pulsars : general; shock waves; supernova remnants; X-rays : general;

D O I：

10.1086/312835

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 fur which case applies and thus plays a role in estimating the pulsar power needed to produce an observed X-ray luminosity.

引用

页码：L45 / L48

页数：4

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