paper

Magnetohydrodynamics in Superconducting-Superfluid Neutron Stars

arXiv:astro-ph/9702032 · doi:10.1046/j.1365-8711.1998.01451.x

Abstract

MHD equations are presented for the mixture of superfluid neutrons, superconducting protons, and normal electrons believed to exist in the outer cores of neutron stars. The dissipative effects of electron viscosity and mutual friction due to electron-vortex scattering are also included. It is shown that Alfven waves are replaced by cyclotron- vortex waves that have not been previously derived from MHD theory. The cyclotron- vortex waves are analogous to Alfven waves with the tension due to the magnetic energy density replaced by the vortex energy density. The equations are then put into a simplified form useful for studying the effects of the interior magnetic field on the dynamics. Of particular interest is the crust-core coupling time which can be inferred from pulsar glitch observations. The hypothesis that cyclotron-vortex waves play a significant role in the core spin-up during a glitch is used to place limits on the interior magnetic field. The results are compared with those of other studies.

11 pages, requires MN plain TeX macros, to appear in MNRAS. Sec. 6 was revised on 02/20/97 to state that stratification will greatly increase the magnetic spin-up time; 09/09/97 version corrects minor typos only

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