http://arxiv.org/abs/1708.07505
The evolution of inclination angle and precession damping of radio pulsars is considered. It is assumed that the neutron star consists of 3 “freely” rotating components: the crust and two core components, one of which contains pinned superfluid vortices. We suppose that each component rotates as a rigid body. Also the influence of the small-scale magnetic field on the star’s braking process is examined. Within the framework of this model the star simultaneously can have glitch-like events combined with long-period precession (with periods $10-10^{4}$ years). It is shown that the case of the small quantity of pinned superfluid vortices seems to be more consistent with observations.
K. Kraav, M. Vorontsov and D. Barsukov
Fri, 25 Aug 17
27/59
Comments: 12 pages, 15 figures
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