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The Mode-Separated Pulse Profiles of Pulsar Radio Emission

Published online by Cambridge University Press:  12 April 2016

Mark M. McKinnon  and
Daniel R. Stinebring
Mark M. McKinnon
Affiliation:
National Radio Astronomy Observatory, Green Bank, WV 24944USA
Daniel R. Stinebring
Affiliation:
Department of Physics, Oberlin College, Oberlin, OH 44074, USA

Abstract

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Two modes of orthogonal polarization are generally observed in the radio emission from pulsars. Essentially all attempts to calculate the average profiles of the individual modes have assumed that the modes occur separately. We have presented evidence, however, that the modes occur simultaneously. Therefore, we believe that “mode-separated” pulse profiles which have been published to date reveal little about the polarization properties of the individual modes.

Calculating mode-separated pulse profiles for superposed orthogonal modes is complicated by the unknown polarization properties of the individual modes. However, the simplest model of pulsar radio emission which can explain the wide variety in the emission’s polarization is one in which the individual modes are completely polarized. We use our simple model to compute the average profiles of the orthogonal modes in PSR B0525+21. The total intensity of the two mode profiles resembles the overall pulse profile, and each profile is highly linearly polarized.

Type
Part 3. Studies of Radio Emission
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 261 - 264
Copyright
Copyright © Astronomical Society of the Pacific 2000

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