Exploring tidal effects of coalescing binary neutron stars in numerical relativity
Exploring tidal effects of coalescing binary neutron stars in numerical relativity
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DOI：
10.1103/physrevd.87.044001
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发表时间：
2013-01
影响因子：
5
通讯作者：
K. Hotokezaka;K. Kyutoku;M. Shibata
中科院分区：
文献类型：
--
作者：
K. Hotokezaka;K. Kyutoku;M. Shibata
我们通过分析数值相对论模拟得到的波形，研究了双星中子星末期发射的引力波。为了从数值结果中提取物理引力波形，分辨率外推在我们的模拟中起着至关重要的作用。将外推的引力波相位与后牛顿(PN)和有效一体(EOB)公式的计算结果进行了比较，其中包括潮汐效应的改正。结果表明，数值相对论中外推的引力波相位与Pn和EOB计算得到的结果在大多数感潮阶段都符合得很好，除了潮汐主导的最终感潮阶段，Pn和EOB的计算结果低估了潮汐效应。然而，在过去的15个周期中，我们的外推结果与Pn/EOB计算结果之间的累积相位差最多只有1-3弧度。
We study gravitational waves emitted in the late inspiral stage of binary neutron stars by analyzing the waveform obtained in numerical-relativity simulations. For deriving the physical gravitational waveforms from the numerical results, the resolution extrapolation plays an essential role for our simulations. The extrapolated gravitational-wave phases are compared with those calculated in the post-Newtonian (PN) and effective-one-body (EOB) formalisms including corrections of tidal effects. We show that the extrapolated gravitational-wave phases in numerical relativity agree well with those by the PN and EOB calculations for most of the inspiral stage except for a tidally-dominated, final inspiral stage, in which the PN and EOB results underestimate the tidal effects. Nevertheless, the accumulated phase difference between our extrapolated results and the results by the PN/EOB calculations is at most 1--3 radian in the last 15 cycles.