Constraining nuclear equations of state using gravitational waves from hypermassive neutron stars.
Constraining nuclear equations of state using gravitational waves from hypermassive neutron stars.
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DOI：
10.1103/physrevlett.94.201101
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发表时间：
2005-04
影响因子：
8.6
通讯作者：
M. Shibata
中科院分区：
文献类型：
--
作者：
M. Shibata
最新的广义相对论模拟结果表明，当中子星的总质量小于与实际物态方程有关的临界值时，在中子星合并后将形成一颗椭球形的超大质量中子星星.来自这种超大质量中子星的准周期引力波的有效振幅在50 Mpc的距离约为6-7 x 10（-21），这可能足够大，可以被先进的激光干涉引力波探测器探测到，尽管频率很高，约为3 kHz。我们指出，此类信号的检测可能会导致对中子星EOS的约束。
Latest general relativistic simulations for the merger of binary neutron stars with realistic equations of states (EOSs) show that a hypermassive neutron star of an ellipsoidal figure is formed after the merger if the total mass is smaller than a threshold value which depends on the EOSs. The effective amplitude of quasiperiodic gravitational waves from such hypermassive neutron stars is approximately 6-7 x 10(-21) at a distance of 50 Mpc, which may be large enough for detection by advanced laser interferometric gravitational wave detectors although the frequency is high, approximately 3 kHz. We point out that the detection of such signals may lead to constraining the EOSs for neutron stars.