Stability and collapse of rapidly rotating, supramassive neutron stars: 3D simulations in general relativity
Stability and collapse of rapidly rotating, supramassive neutron stars: 3D simulations in general relativity
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快速旋转的超大质量中子星的稳定性和坍缩：广义相对论中的 3D 模拟
DOI：
10.1103/physrevd.61.044012
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发表时间：
1999
影响因子：
5
通讯作者：
S. Shapiro
中科院分区：
文献类型：
--
作者：
M. Shibata;T. Baumgarte;S. Shapiro
我们在完全广义相对论中进行了三维数值模拟，以研究快速旋转的超大质量中子星在质量剥离极限到动力学崩塌时的稳定性。我们采用G52的绝热状态方程，聚焦于均匀自转的恒星。我们发现，沿质量脱落序列的动力学不稳定性的开始与长期不稳定性的开始几乎重合。不稳定的恒星在大约一个自转周期内崩塌为旋转的黑洞。我们还研究了由于压力耗尽而变得不稳定的稳定恒星的崩塌，例如，通过相变！或者说是大量的吸积。在任何情况下，我们都没有找到在新形成的克尔黑洞周围形成大质量圆盘或任何喷射物的证据，即使前身正在快速旋转。
We perform 3D numerical simulations in full general relativity to study the stability of rapidly rotating, supramassive neutron stars at the mass-shedding limit to dynamical collapse. We adopt an adiabatic equation of state with G52 and focus on uniformly rotating stars. We find that the onset of dynamical instability along mass-shedding sequences nearly coincides with the onset of secular instability. Unstable stars collapse to rotating black holes within about one rotation period. We also study the collapse of stable stars which have been destabilized by pressure depletion ~e.g., via a phase transition! or mass accretion. In no case do we find evidence for the formation of massive disks or any ejecta around the newly formed Kerr black holes, even though the progenitors are rapidly rotating.