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On the precession of the isolated pulsar PSR B1828-11

By Vahid Rezania


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, 250, and 167 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-component (Link & Epstein 2001). In this paper, we show that if the dipole moment vector varies with time with a period nearly equal to the longest (probably fundamental) observed period ( ≃ 1000 d), the magnetic dipole torque may produce the all other harmonics. We find the second and fourth harmonics at periods ≃ 500 and 250 d are dominant for small wobble angle ≃ 3 ◦ and large field’s inclination angle � 89 ◦. Further, in a good agreement with data, we model the changes of the pulse shape in the precession cycle and find that the variation of pulse duration follows from a standard beam pattern in this cycle. Subject headings: pulsar: individual(PSR B1828-11) – stars: neutron – stars: magnetic fields 1

Year: 2002
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