Radiation pattern of the isolated pulsar PSR B 1828 - 11
نویسنده
چکیده
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 standard beam pattern in each cycle.
منابع مشابه
ar X iv : a st ro - p h / 02 05 18 0 v 2 1 5 M ay 2 00 2 On the precession of the isolated pulsar PSR B 1828 - 11
Analysis of both pulse timing and pulse shape variations of the isolated pulsar PSR B1828-11 shows highly correlated and strong Fourier power at periods ≃ 1000, 500, and 250 d (Stairs et al. 2000). The only description based on a free precession of star’s rigid crust coupled to the magnetic dipole torque, explains the 500-component, as the fundamental Fourier frequency, with its harmonic 250-co...
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Analysis of both pulse timing and pulse shape variations of the isolated pulsar PSR B1828-11 shows highly correlated and strong Fourier power at periods ≃ 1000, 500, and 250 d (Stairs et al. 2000). The only description based on a free precession of star’s rigid crust coupled to the magnetic dipole torque, explains the 500-component, as the fundamental Fourier frequency, with its harmonic 250com...
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