A numerical study of the r-mode instability of rapidly rotating nascent neutron stars

Shin'ichirou Yoshida, Shigeyuki Karino, Shijun Yoshida, Yoshiharu Eriguchi

研究成果: Article査読

13 被引用数 (Scopus)

抄録

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.

本文言語English
ページ(範囲)L1-L4
ジャーナルMonthly Notices of the Royal Astronomical Society
316
1
DOI
出版ステータスPublished - 2000 7 21

ASJC Scopus subject areas

  • 天文学と天体物理学
  • 宇宙惑星科学

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