Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..apr4a4003l&link_type=abstract
American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As
Astronomy and Astrophysics
Astrophysics
Scientific paper
Pulse timing of the isolated pulsar PSR B1828-11 shows strong Fourier power at periods ~= 1000, 500 and 250 d, correlated with changes in the pulse profile. I present a model of precession of a biaxial stellar crust, coupled to magnetic dipole torque, with which to interpret these data. Within this model, the correlated changes in the pulse duration and spin period derivative can be explained as precession at a period of ~= 500 d with a wobble angle of ~= 3^circ, provided the star's dipole moment is nearly orthogonal to the crust's symmetry axis. The dipole torque produces a harmonic at ~= 250 d. Comparison of the predicted spin dynamics with the observed pulse durations implies that the radio beam has a non-standard ``hour-glass" shape. If the precession interpretation is correct, the neutron vortices expected to exist in the inner crust cannot be pinned. In support of this conclusion, I describe how hydrodynamic forces present in a precessing star are likely to prevent vortex pinning almost everywhere in the crust.
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