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Magnetic effects on the viscous boundary layer damping of the r-modes in neutron stars

Gregory Mendell
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Abstract

This paper explores the effects that magnetic fields have on the viscous boundary layers (VBLs) that can form in neutron stars at the crust-core interface, and it investigates the VBL damping of the gravitational-radiation driven r-mode instability. Approximate solutions to the magnetohydrodynamic equations valid in the VBL are found for ordinary-fluid neutron stars. It is shown that magnetic fields above 10^9 Gauss significantly change the structure of the VBL, and that magnetic fields decrease the VBL damping time. Furthermore, VBL damping completely suppresses the r-mode instability for B >= 10^{12} Gauss. Thus, magnetic fields will profoundly affect the VBL damping of the r-mode instability in hot young pulsars (that are cool enough to have formed a solid crust). One can speculate that magnetic fields can affect the VBL damping of this instability in LMXBs and other cold old pulsars (if they have sufficiently large internal fields).

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Gregory Mendell. 2001-02-09. Magnetic effects on the viscous boundary layer damping of the r-modes in neutron stars. https://doi.org/10.1103/physrevd.64.044009

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