2008/07/31 by A. Passamonti, B. Haskell, N. Andersson +2 · 1 citation
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Geophysics and Sensor Technology #Pulsars and Gravitational Waves Research #astro-ph #gr-qc
paper · pdf · doi:10.1111/j.1365-2966.2009.14408.x
16 pages, 12 figures, 4 tables, corrected Table 1
openalex publication_date 2009/03/03 · arxiv created 2009/03/26 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We use time-evolutions of the linear perturbation equations to study the oscillations of rapidly rotating neutrons stars. Our models account for the buoyancy due to composition\ngradients and we study, for the first time, the nature of the resultant g-modes in a fast spinning star. We provide detailed comparisons of non-stratified and stratified models. This leads to an improved understanding of the relationship between the\ninertial modes of a non-stratified star and the g-modes of a stratified system. In particular, we demonstrate that each g-mode becomes rotation-dominated, i.e. approaches\na particular inertial mode, as the rotation rate of the star is increased. We also discuss issues relating to the gravitational-wave driven instability of the various classes of oscillation modes.