Triplicity of pulsar profiles and orthogonal polarization modes

Journal Article · Wed Oct 01 04:00:00 EDT 1986 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/164629· OSTI ID:6640804

Gil, J

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. 17 references.

• Research Organization: Kentucky Univ., Lexington
• OSTI ID: 6640804
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 309; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
COSMIC RADIO SOURCES
MAGNETIC FIELDS
POLARIZATION
PULSARS
STELLAR ATMOSPHERES
STELLAR MAGNETOSPHERES
STELLAR RADIATION