EDP Sciences
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Volume 399, Number 2, February IV 2003
Page(s) 659 - 662
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20021755

A&A 399, 659-662 (2003)
DOI: 10.1051/0004-6361:20021755

Radiation pattern of the isolated pulsar PSR B1828-11

V. Rezania

Institute for Advanced Studies in Basic Sciences, Gava Zang, Zanjan 45195, Iran
(Received 9 September 2002 / Accepted 25 November 2002 )

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 $\simeq$500 d. Recent theoretical studies suggested that the actual precession period might be $\simeq$1000 d as seen in observations (Rezania 2003; 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 $\simeq$1000 d and find that the variation of the pulse duration follows from a standard beam pattern in each cycle.

Key words: pulsar: individual: PSR B1828-11 -- stars: neutron

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