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Pulsar Winds

Published online by Cambridge University Press:  12 April 2016

Jonathan Arons
Jonathan Arons*
Affiliation:
University of California

Abstract

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The shock excitation of pulsar powered nebulae (plerions) is discussed, based on recent theoretical work on the structure of relativistic, collisionless magnetosonic shock waves. This theory is used to outline a model in which the γ−2 injection spectrum of the Crab Nebula is satisfactorily accounted for. The same theory suggests a model of the “wisp” features in the Crab Nebula which accounts for these time variable features in the surface bightness as compressions associated with the magnetic overshoots within the shock structure. It is pointed out that this theory suggests observable variability in the high energy gamma rays from the Crab Nebula (ε > 50 MeV).

Type
Part 6 Winds and the ISM
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 401 - 408
Copyright
Copyright © Astronomical Society of the Pacific 1996

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