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Collimation and Dissipation of Pulsar Winds

Published online by Cambridge University Press:  25 April 2016

Tzihong Chiueh
Tzihong Chiueh*
Affiliation:
Institute of Physics and Astronomy, National Central University, Chung-Li, Taiwan, ROC
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Abstract

A nearly stationary pulsar wind is shown to be always collimating along the direction of rotation. It follows that the conventional picture of the equatorial pulsar wind can occur only in a highly time-dependent manner, which, if true, may account for the observed time variation within a single pulse. Furthermore, a mechanism, via excitation of magnetosolitons, is proposed for explaining the continuous generation of energetic electrons, which yield the observed radio emission in the Type II supernova remnants. Fully relativistic analyses will be presented to substantiate these claims.

Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 9 , Issue 1 , 1991 , pp. 137
Copyright
Copyright © Astronomical Society of Australia 1991

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