Pulsar beam orientation

Details Pulsar beam orientation Pulsar beam orientation

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985azh....62..240g&link_type=abstract

(Astronomicheskii Zhurnal, vol. 62, Mar.-Apr. 1985, p. 240-251) Soviet Astronomy (ISSN 0038-5301), vol. 29, Mar.-Apr. 1985, p. 1

Astronomy and Astrophysics

Astronomy

1

Beams (Radiation), Pulsars, Stellar Radiation, Circular Polarization, Elliptical Polarization, Polarization (Waves), Stellar Magnetic Fields, Stellar Rotation

Scientific paper

One of the important problems in the pulsar investigation is to determine the intrinsic width of the radiation beam (2Θ), the angle α between the magnetic axis and the rotation axis, and their time evolution. The authors made an attempt to solve this problem concerning not every concrete pulsar, but PSRs as a whole. They selected the pulsars with well-determined estimates of the maximum velocity of the change in the polarization plane. The angle α and the intrinsic width of the radiation diagram (2Θ) turned out to undergo considerable changes in time by a factor of ≡5. This naturally leads to a great difference in the probability of detecting young and old pulsars. The probability of detecting PSRs with interpulses is also considered.

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