1999/10/31 by Shin'ichirou Yoshida, Shigeyuki Karino, S. Karino +4 · 2 citations
Engineering · Physics and Astronomy · #Cosmology and Gravitation Theories #Geophysics and Sensor Technology #Pulsars and Gravitational Waves Research #astro-ph #gr-qc
paper · pdf · doi:10.1046/j.1365-8711.2000.03698.x
published as Mon.Not.Roy.Astron.Soc. 316 (2000) L1 · 4 pages, 2 figures; MNRAS,316,L1(2000)
openalex publication_date 2000/07/21 · arxiv created 2000/08/10 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
The first results of numerical analysis of classical r-modes of rapidly rotating compressible stellar models are reported. The full set of linear perturbation equations of rotating stars in Newtonian gravity is solved numerically without the slow rotation approximation. A critical curve of gravitational wave emission induced instability, which restricts the rotational frequencies of hot young neutron stars, is obtained. Taking the standard cooling mechanisms of neutron stars into account, we also show the ‘evolutionary curves’ along which neutron stars are supposed to evolve as cooling and spinning down proceed. Rotational frequencies of 1.4-M⊙ stars suffering from this instability decrease to around 100 Hz when the standard cooling mechanism of neutron stars is employed. This result confirms the results of other authors, who adopted the slow rotation approximation.