paper

Hydrodynamic Stability Analysis of the Neutron Star Core

arXiv:1806.00967 · doi:10.3847/1538-4357/aacc24

Abstract

Hydrodynamic instabilities and turbulence in neutron stars have been suggested to be related to observable spin variations in pulsars, such as spin glitches, timing noise, and precession (nutation). Accounting for the stabilizing effects of the stellar magnetic field, we revisit the issue of whether the inertial modes of a neutron star can become unstable when the neutron and proton condensates flow with respect to one another. The neutron and proton condensates are coupled through the motion of imperfectly pinned vorticity (vortex slippage) and vortex-mediated scattering (mutual friction). Two-stream instabilities that occur when the two condensates rotate with respect to one another in the outer core are stabilized by the toroidal component of the magnetic field. This stabilization occurs when the Alfvén speed of the toroidal component of the magnetic field becomes larger than the relative rotational velocity of the condensates, corresponding to toroidal field strengths in excess of . In contrast with previous studies, we find that spin down of a neutron star under a steady torque is stable. The Donnelly--Glaberson instability is not stabilized by the magnetic field, and could play an important role if neutron stars undergo precession.

arXiv comment38 pages, 7 figures, submitted to ApJ

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