Gravitational waves from relativistic neutron-star mergers with microphysical equations of state.
Gravitational waves from relativistic neutron-star mergers with microphysical equations of state.
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相对论中子星合并产生的引力波与微物理状态方程
DOI：
10.1103/physrevlett.99.121102
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发表时间：
2007
影响因子：
8.6
通讯作者：
H.-Th. Janka
中科院分区：
文献类型：
--
作者：
R. Oechslin;H.-Th. Janka
分析了一组相对论中子星（NS）合并模拟的引力波（GW）发射，并识别了特征信号特征。GW能谱中与超大质量合并残留物形成相关的明显峰值的频率强烈依赖于核状态方程（EOS）的性质和二元系统的总质量，而质量比和NS自旋的影响很弱。如果总质量可以从螺旋啁啾信号确定，则合并后信号的峰值频率是EOS的敏感指标。
The gravitational wave (GW) emission from a set of relativistic neutron-star (NS) merger simulations is analyzed and characteristic signal features are identified. The distinct peak in the GW energy spectrum that is associated with the formation of a hypermassive merger remnant has a frequency that depends strongly on the properties of the nuclear equation of state (EOS) and on the total mass of the binary system, whereas the mass ratio and the NS spins have a weak influence. If the total mass can be determined from the inspiral chirp signal, the peak frequency of the post-merger signal is a sensitive indicator of the EOS.