Dynamical instability of differentially rotating stars
Dynamical instability of differentially rotating stars
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差分旋转恒星的动力学不稳定性
DOI：
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发表时间：
2002
期刊：
影响因子：
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通讯作者：
Y. Eriguchi
中科院分区：
文献类型：
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作者：
M. Shibata;S. Karino;Y. Eriguchi
我们研究了不同自转恒星对棒模形变的动力学不稳定性。采用多方指数n= 1的多方状态方程进行了数值模拟和线性微扰分析。结果表明，即使动能与引力势能之比为O（0.01），高度差旋的旋转恒星也是动力学不稳定的。用四极公式计算了末态非轴对称准定态的引力波。对于质量为1.4 M <$m，半径为10 km的旋转恒星，引力波的频率为100 Hz，有效振幅为105 × 10−22，距离为100 Mpc。
We study the dynamical instability against bar-mode deformation of differentially rotating stars. We performed numerical simulation and linear perturbation analysis adopting polytropic equations of state with the polytropic index n= 1. It is found that rotating stars of a high degree of differential rotation are dynamically unstable even for the ratio of the kinetic energy to the gravitational potential energy of O(0.01). Gravitational waves from the final non-axisymmetric quasi-stationary states are calculated in the quadrupole formula. For rotating stars of mass 1.4 M⊙ and radius several 10 km, gravitational waves have frequency several 100 Hz and effective amplitude ∼5 × 10−22 at a distance of ∼100 Mpc.