1998/06/30 by Dong Lai · 2 citations
Earth and Planetary Sciences · Engineering · Physics and Astronomy · #Geophysics and Gravity Measurements #Geophysics and Sensor Technology #Pulsars and Gravitational Waves Research #astro-ph #gr-qc
paper · pdf · doi:10.1046/j.1365-8711.1999.02723.x
published as Mon.Not.Roy.Astron.Soc.307:1001-1007,1999 · 8 pages, 5 figures; MNRAS, in press. 2 figures added; More details are given for the mode properties
arxiv created 1999/04/09 · openalex publication_date 1999/08/01 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/30
Gravitational radiation tends to drive gravity modes in rotating neutron stars to become unstable. For an inviscid star, the instability sets in when the rotation frequency is about 0.7 times the corresponding mode frequency of the non-rotating star. Neutron stars with spin frequencies ≳100Hz are susceptible to this instability, with a growth time of the order of years. However, it is likely that viscous dissipation suppresses the instability except for a narrow range of temperatures around 109K. We also show that the viscosity-driven instability of g-modes is absent.