Inferring the neutron star equation of state from binary inspiral waveforms
Inferring the neutron star equation of state from binary inspiral waveforms
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DOI：
10.1142/9789814374552_0046
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发表时间：
2010-08
期刊：
影响因子：
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通讯作者：
C. Markakis;J. Read;M. Shibata;K. Uryū;J. Creighton;J. Friedman
中科院分区：
文献类型：
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作者：
C. Markakis;J. Read;M. Shibata;K. Uryū;J. Creighton;J. Friedman
在核密度以上的中子星物质的性质还不完全清楚。双中子星在吸气和合并的后期阶段发出的引力波包含了中子星状态方程的印记。测量从后期激励波形的点粒子极限的偏离，可以通过引力波观测来测量状态方程的性质。这篇论文和j.s. Read的演讲报告了从激发中子星双星模拟中得到的数值波形的比较，计算了不同刚度的状态方程。我们计算了各种委托和建议的干涉引力波探测器的波形差异的信号强度，并表明在1 kHz左右的频率上的观测将能够测量紧凑性参数并约束可能的中子星状态方程。
The properties of neutron star matter above nuclear density are not precisely known. Gravitational waves emitted from binary neutron stars during their late stages of inspiral and merger contain imprints of the neutron-star equation of state. Measuring departures from the point-particle limit of the late inspiral waveform allows one to measure properties of the equation of state via gravitational wave observations. This and a companion talk by J. S. Read reports a comparison of numerical waveforms from simulations of inspiraling neutron-star binaries, computed for equations of state with varying stiffness. We calculate the signal strength of the difference between waveforms for various commissioned and proposed interferometric gravitational wave detectors and show that observations at frequencies around 1 kHz will be able to measure a compactness parameter and constrain the possible neutron-star equations of state.