用第三代引力波探测器约束中子星的物态方程
Constraining the Equation of State of Neutron Stars with third-generation Gravitational Wave detectors
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中文总结 AI 辅助
本研究利用第三代引力波探测器模拟信号，通过Fisher矩阵分析发现事件数量增加可收紧中子星物态方程约束，且质量分布影响更大，均匀分布优于双峰分布，亚太阳质量中子星能显著降低亚饱和密度区不确定性。
中文摘要 AI 辅助
我们研究了双中子星并合事件数量和中子星（NS）质量分布对约束物态方程（EoS）、潮汐形变度、中子星半径以及核参数的影响，使用的是第三代探测器探测到的双中子星旋进引力波信号。在给定事件数量和质量分布模型后，我们生成模拟引力波信号，并计算每个事件的Fisher信息矩阵。通过将非EoS波形参数固定在其注入值上，并累积所有事件的Fisher矩阵，得到EoS参数的协方差。最后，基于该协方差矩阵生成EoS、潮汐形变度、半径和核参数的后验样本。我们发现，由于观测事件更多和数据积累，事件数量越多约束越紧，这与探测数量增加带来的预期一致。同时，我们注意到质量分布在约束EoS中起着更重要的作用。我们比较了现实的双峰高斯分布、均匀分布以及包含亚太阳质量中子星的另一种均匀分布。结果表明，均匀分布比双峰模型产生更紧的约束，因为它包含了更多低质量和大质量中子星。这也意味着接近$1.4\\,\Msun$的事件提供了关于EoS的部分冗余信息。此外，包含亚太阳质量中子星可以通过显著降低亚饱和密度和内壳层的EoS不确定性来进一步改善约束，凸显了亚饱和密度EoS的重要性。
英文摘要
We investigated the impact of the number of binary neutron star merger events and neutron star (NS) mass distributions on constraining the equation of state (EoS), tidal deformability and radius of NSs, as well as the nuclear parameters, using binary neutron star inspiral gravitational wave signals with third-generation detectors. We generate simulated gravitational wave signals and compute the Fisher information matrix for each event after the number of events and mass distribution models are given. The covariance of EoS parameters is obtained by holding the non-EoS waveform parameters fixed at their injected values and accumulating the Fisher matrix over all events. Finally, the posterior samples of EoS, tidal deformability, radius and nuclear parameters are generated based on this covariance matrix. We find that larger number of events lead to tighter constraints due to more observed events and data accumulation, as expected given the increased number of detections. Meanwhile, we note that the mass distribution plays a more important role in constraining the EoS. We compare a realistic bimodal Gaussian distribution, a uniform distribution and another uniform including sub-solar mass NSs. The results show that the uniform distribution yields tighter constraints than bimodal models because it includes more low-mass and massive NSs. This also implies that events near $1.4\,\Msun$ provide partly redundant information about the EoS. Additionally, including sub-solar mass NSs can further improve the constraints by significantly reducing the EoS uncertainties at sub-saturation densities and inner-crust, highlighting the importance of sub-saturation density EoS.
发表机构
- Rochester Institute of Technology（罗切斯特理工学院）
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