Abstract
The forced motion of superfluid vortices in shear oscillations of rotating solid neutron star matter produces damping of the mode. A simple model of the unpinning and repinning processes is described, with numerical calculations of the consequent energy decay times. These are of the order of 1 s for typical anomalous X-ray pulsars with rotational angular velocity Ω≈ 1 rad s−1 but become very short for radio pulsars with Ω≈ 10–100 rad s−1. The superfluid friction processes considered here may also be significant for the damping of r modes in rapidly rotating neutron stars.
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