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Wave propagation in pulsar magnetospheres

Published online by Cambridge University Press:  20 March 2013

Chen Wang ,
Dong Lai  and
Jinlin Han
Chen Wang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences. A20 Datun Road, Chaoyang District, Beijing 100012, China email: wangchen@nao.cas.cn, hjl@nao.cas.cn
Dong Lai
Affiliation:
Department of Astronomy, Cornell University, Ithaca, NY 14853, USA email: dong@astro.cornell.edu
Jinlin Han
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences. A20 Datun Road, Chaoyang District, Beijing 100012, China email: wangchen@nao.cas.cn, hjl@nao.cas.cn
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Abstract

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We study the propagation effects of radio waves in a pulsar magnetosphere, composed of relativistic electron-positron pair plasmas streaming along the magnetic field lines and corotating with the pulsar. We critically examine the various physical effects that can potentially influence the observed wave intensity and polarization. We numerically integrate the transfer equations for wave polarization in the rotating magnetosphere, taking account of all the propagation effects in a self-consistent manner. For typical magnetospheric plasma parameters produced by pair cascade, we find that the observed radio intensity and polarization profiles can be strongly modified by the propagation effects. Some applications of our results are discussed.

Keywords

pulsars: generalplasmaspolarizationmagnetic fieldsradiative transfer
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 540 - 542
Copyright
Copyright © International Astronomical Union 2013

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