The use of hypermodels to understand binary neutron star collisions
The use of hypermodels to understand binary neutron star collisions
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DOI：
10.1038/s41550-022-01707-x
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发表时间：
2022-07
期刊：
影响因子：
14.1
通讯作者：
G. Ashton;T. Dietrich
中科院分区：
文献类型：
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作者：
G. Ashton;T. Dietrich
来自双中子星碰撞的引力波为研究超核物质的行为、引力的基本性质和我们宇宙的宇宙历史提供了一个独特的机会。然而，由于爱因斯坦场方程的复杂性，使得能够进行源属性推断的理论模型由于简化假设而遭受系统不确定性。我们开发了一个超模型的方法来比较和测量的不确定性引力波近似。使用国家的最先进的模型，我们应用这种新技术的二元中子星星观测GW 170817和GW 190425和亚阈值候选人GW 200311_103121。我们的分析揭示了波形模型之间微妙的系统差异，频率依赖性研究表明，这是由于潮汐部门的治疗。这种新技术为模型开发提供了一个试验场，并在未来的观测运行中识别波形系统学，其中探测器的改进将增加我们观察到的二元中子星星碰撞的数量和清晰度。
Gravitational waves from the collision of binary neutron stars provide a unique opportunity to study the behaviour of supranuclear matter, the fundamental properties of gravity, and the cosmic history of our Universe. However, given the complexity of Einstein's Field Equations, theoretical models that enable source-property inference suffer from systematic uncertainties due to simplifying assumptions. We develop a hypermodel approach to compare and measure the uncertainty gravitational-wave approximants. Using state-of-the-art models, we apply this new technique to the binary neutron star observations GW170817 and GW190425 and the sub-threshold candidate GW200311_103121. Our analysis reveals subtle systematic differences between waveform models, and a frequency-dependence study suggests that this is due to the treatment of the tidal sector. This new technique provides a proving ground for model development, and a means to identify waveform-systematics in future observing runs where detector improvements will increase the number and clarity of binary neutron star collisions we observe.