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

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

Research output: Contribution to journalArticlepeer-review

13 Citations (Scopus)


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.

Original languageEnglish
Pages (from-to)L1-L4
JournalMonthly Notices of the Royal Astronomical Society
Issue number1
Publication statusPublished - 2000 Jul 21


  • Stars: neutron
  • Stars: oscillations
  • Stars: rotation

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


Dive into the research topics of 'A numerical study of the r-mode instability of rapidly rotating nascent neutron stars'. Together they form a unique fingerprint.

Cite this