Volume 399, Number 2, February IV 2003
|Page(s)||659 - 662|
|Section||Stellar structure and evolution|
|Published online||07 February 2003|
Radiation pattern of the isolated pulsar PSR B1828-11
Institute for Advanced Studies in Basic Sciences, Gava Zang, Zanjan 45195, Iran
Corresponding author: firstname.lastname@example.org
Accepted: 25 November 2002
Based on the free precession model of the isolated pulsar PSR B1828-11, Link & Epstein ([CITE]) 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 [CITE]; Wasserman [CITE]). In this paper, in a good agreement with the observed data (Stairs et al. [CITE]), 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 standard beam pattern in each cycle.
Key words: pulsar: individual: PSR B1828-11 / stars: neutron
© ESO, 2003
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