## 抄録

We investigate the instability driven by viscosity in rotating relativistic stars by means of an iterative approach. We focus on polytropic rotating equilibrium stars and impose an m=2 perturbation in the lapse. We vary both the stiffness of the equation of state and the compactness of the star to study these factors on the critical value T/W for the instability. For a rigidly rotating star, the criterion T/W, where T is the rotational kinetic energy and W the gravitational binding energy, mainly depends on the compactness of the star and takes values around 0.13-0.16, which slightly differ from that of Newtonian incompressible stars (∼0.14). For differentially rotating stars, the critical value of T/W is found to span the range 0.17-0.25. The value is significantly larger than in the rigidly rotating case with the same compactness of the star. Finally we discuss the possibility of detecting gravitational waves from viscosity-driven instabilities using ground-based interferometers.

本文言語 | English |
---|---|

ページ（範囲） | 481-485 |

ページ数 | 5 |

ジャーナル | Astrophysics and Space Science |

巻 | 308 |

号 | 1-4 |

DOI | |

出版ステータス | Published - 2007 4月 |

外部発表 | はい |

## ASJC Scopus subject areas

- 天文学と天体物理学
- 宇宙惑星科学