The pulsar PSR B1931+24 as an orthogonal rotator

Details The pulsar PSR B1931+24 as an orthogonal rotator The pulsar PSR B1931+24 as an orthogonal rotator

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007arep...51..477m&link_type=abstract

Astronomy Reports, Volume 51, Issue 6, pp.477-480

Astronomy and Astrophysics

Astronomy

97.60.Gb, 97.10.Kc

Scientific paper

The angles of the magnetic moment µ and the line of sight L to the rotation axis Ω are estimated for the pulsar PSR B1921+24, which displays “on” and “off” periods in its radio emission. It is shown that this object is an orthogonal rotator, i.e., the angle β between µ and Ω is equal to 88°.2 and the angle between L and Ω is ζ = 98.7°, and that its rotation period should be twice the usually adopted value (P = 1.626 s). One possible reason for the peculiarities of this pulsar could be the precession of a relic disk in the equatorial region of the object. Further observations (in particular, in the infrared) are required to confirm the existence of such a disk. Polarization data for other pulsars whose radiation switches on and off (transients) are also required, to determine if they are likewise orthogonal rotators. Calculations for PSR B0656+14 show that β ˜ 20°, and the sharp increase of its pulse intensities is due to intrinsic reasons, and is not associated with a relic disk.

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