Vortex repinning in neutron star crusts

Details Vortex repinning in neutron star crusts Vortex repinning in neutron star crusts

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277..225s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 1, pp. 225-234.

Astronomy and Astrophysics

Astronomy

6

Hydrodynamics, Stars: Neutron, Stars: Rotation

Scientific paper

Repinning of superfluid neutron vortices to the lattice nuclei in neutron star crusts is examined within a superfluid hydrodynamic approach. The equations of motion of a vortex in the pinning potential field of a nucleus are obtained and solved for the case of a parabolic potential. The vortex repinning depends on the strength of the pinning potential, on the magnitude of the viscous friction coefficient in the free vortex flow regime, and, less sensitively, on the impact angle. A numerical evaluation, using the rotation period of the Vela pulsar, shows that repinning is possible in the bulk of the crust if the largest of the currently estimated values of the viscous friction coefficient and a moderate-strength pinning potential are adopted. For smaller values of the parameters, repinning is possible only in rather localized regions, preferably for large values of the impact angle.

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