Radiation pattern of the isolated pulsar PSR B1828-11

Details Radiation pattern of the isolated pulsar PSR B1828-11 Radiation pattern of the isolated pulsar PSR B1828-11

2002-11-18

arxiv.org/abs/astro-ph/0211410v1

Astron.Astrophys. 399 (2003) 659

Astronomy and Astrophysics

Astrophysics

9 pages, 3 figures, Accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20021755

Based on the free precession model of the isolated pulsar PSR B1828-11, Link & Epstein 2001) showed that the observed pulse durations require the radio beam to have a non-standard shape: the beam duration is larger for beam sweeps farthest from the dipole axis. In their analysis they assumed that the actual precession period is ~ 500 d. Recent theoretical studies suggested that the actual precession period might be ~ 1000 d as seen in observations (Rezania 2002, Wasserman 2002). In this paper, in a good agreement with the observed data (Stairs et al. 2000), we model the changes of the pulse shape in a precession cycle with period ~ 1000 d and find that the variation of the pulse duration follows from a {\it standard} beam pattern in each cycle.

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