A ray-tracing model of the Vela magnetosphere

被引：0

作者：

Hirano, C ^{[1
]}

Gwinn, CR ^{[1
]}

机构：

[1] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

来源：

PULSAR ASTRONOMY - 2000 AND BEYOND: IAU COLLOQUIUM 177 | 2000年 / 202卷

关键词：

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In the relativistic plasma surrounding a pulsar, a subluminal ordinary-mode electromagnetic wave will propagate along a magnetic field line. After some distance, it can break free of the field line and escape the magnetosphere to reach an observer. We apply a simple model of pulsar radio emission based on this scenario to the case of the Vela pulsar and find it reproduces some qualitative characteristics of the observed Vela pulse profile.

引用

页码：437 / 438

页数：2