2003/01/07 by P. B. Jones
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysical Phenomena and Observations #Earth Systems and Cosmic Evolution #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2003.06288.x
published as Mon.Not.Roy.Astron.Soc. 340 (2003) 247 · 7 LaTeX pages, 4 eps figures; accepted for publication in MNRAS
arxiv created 2003/01/07 · openalex publication_date 2003/03/21 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
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.