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A Ray-Tracing Model of the Vela Magnetosphere

Published online by Cambridge University Press:  12 April 2016

C. Hirano  and
C. R. Gwinn
C. Hirano
Affiliation:
Department of Physics, University of California, Santa Barbara, CA 93106
C. R. Gwinn
Affiliation:
Department of Physics, University of California, Santa Barbara, CA 93106

Abstract

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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.

Type
Part 6. Emission and Plasma Theory
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 437 - 438
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Barnard, J.J., & Arons, J. 1986, ApJ, 302, 138 Google Scholar
Gallant, Y.A. 1996, in IAU Colloq. 160, Pulsars: Problems and Progress, ed. Johnston, S., Walker, M.A., and Bailes, M. (San Francisco: Astronomical Society of the Pacific), 431 Google Scholar