Other
Scientific paper
Oct 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...309..609g&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 309, Oct. 15, 1986, p. 609-618. Research supported by the Polska Akademia N
Other
10
Polarization Characteristics, Polarized Electromagnetic Radiation, Pulsars, Stellar Radiation, Angles (Geometry), Orthogonality, Stellar Magnetic Fields
Scientific paper
It is assumed that pulsar emission is composed of two distinct beams originating in the magnetosphere at widely separated locations. It is shown that if one of the beams arises in a region where the magnetic field lines are distorted from dipolar form due to the pulsar rotation then the polarization vectors of this beam are not, in general, parallel to the polarization vectors of the other beam which originates in an undistorted field region. In many geometrical situations, the polarization vectors of the two distinct beams can be mutually quasi-perpendicular. Therefore, the existence of these two beams of pulsar emission is equivalent to the existence of two superposed orthogonal polarization modes. It is argued that different polarization modes correspond to the core and conal pulsar emission. The main polarization mode associated with core emission originates close to the star, while the other mode associated with conal emission originates much farther from the star, in the region where the curvature of the field lines is dominated by the toroidal component of the pulsar magnetic field.
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