Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981pazh....7..731o&link_type=abstract
(Pis'ma v Astronomicheskii Zhurnal, vol. 7, Dec. 1981, p. 731-735.) Soviet Astronomy Letters, vol. 7, Nov.-Dec. 1981, p. 404-406
Astronomy and Astrophysics
Astronomy
4
Orthogonality, Polarization Characteristics, Propagation Modes, Pulsar Magnetospheres, Pulsars, Radio Emission, Stellar Winds, Circular Polarization, Electron Plasma, Polarized Radiation, Relativistic Plasmas, Stellar Magnetic Fields, Stellar Models, Wave Propagation
Scientific paper
The effects of plasma in the pulsar magnetosphere on radiation parameters are considered, under the assumption that the radio emission frequency is much less than the Langmuir frequency. The propagation of radio waves through the relativistic plasma of the pulsar magnetosphere is traced. It is demonstrated that in dense magnetospheric plasma, fast magnetoacoustic wave propagation will occur whereas the group velocity vector of the Alfven wave will be directed along the exterior magnetic field. These two waves will experience a mutually orthogonal polarization. In addition, a model is presented which explains the following four orthogonal mode features: (1) strong linear polarization is exhibited in individual subpulses, (2) the polarization position angle jumps by 90 degrees between subpulses, (3) the circular polarization reverses sign with the angle position change, and (4) the spacing and width of the subpulses depend weakly on the frequency.
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