Bayesian Analysis of Neutron-star Properties with Parameterized Equations of State: The Role of the Likelihood Functions
Bayesian Analysis of Neutron-star Properties with Parameterized Equations of State: The Role of the Likelihood Functions
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用参数化状态方程对中子星特性进行贝叶斯分析：似然函数的作用
DOI：
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发表时间：
2022
影响因子：
4.9
通讯作者：
L. Rezzolla
中科院分区：
文献类型：
--
作者：
Jin;C. Ecker;L. Rezzolla
我们已经调查了系统的差异时，进行贝叶斯推理分析的状态方程（EOS）的中子星采用可变或恒定的似然函数。前者的优点是保留了测量值分布的全部信息，可以充分利用数据。另一方面，后者具有更简单的实现和降低的计算成本的优点。在这两种方法中，EOS具有相同的先验，并已建立使用声速参数化方法，以满足约束条件，从X射线和引力波观测，以及那些从手征有效理论和微扰量子色动力学。在所有情况下，这两种方法导致非常相似的结果，90%的置信水平基本上重叠。有些差异确实出现了，但在概率密度非常小的区域，主要是由于在常似然方法中设置的二元潮汐变形能力Λ ε ≤720的急剧截止。我们的分析还产生了另外两个结果。第一，归一化中心数密度，n c，TOV/n s，和最大质量星星的半径，R TOV之间的负相关。其次，也是最重要的一点，它证实了啁啾质量与双星潮汐变形能力之间的关系。这一结果的重要性在于，它将非常精确测量的λ啁啾与包含EOS重要信息的Λ啁啾联系起来。因此，当在未来的检测中测量到λ啁啾时，我们的关系可以用于对Λ啁啾设置严格的约束。
We have investigated the systematic differences introduced when performing a Bayesian-inference analysis of the equation of state (EOS) of neutron stars employing either variable- or constant-likelihood functions. The former has the advantage of retaining the full information on the distributions of the measurements, making exhaustive usage of the data. The latter, on the other hand, has the advantage of a much simpler implementation and reduced computational costs. In both approaches, the EOSs have identical priors and have been built using the sound speed parameterization method so as to satisfy the constraints from X-ray and gravitational waves observations, as well as those from chiral effective theory and perturbative quantum chromodynamics. In all cases, the two approaches lead to very similar results and the 90% confidence levels essentially overlap. Some differences do appear, but in regions where the probability density is extremely small and are mostly due to the sharp cutoff on the binary tidal deformability Λ˜≤720 set in the constant-likelihood approach. Our analysis has also produced two additional results. First, an inverse correlation between the normalized central number density, n c,TOV/n s , and the radius of a maximally massive star, R TOV. Second, and most importantly, it has confirmed the relation between the chirp mass and the binary tidal deformability. The importance of this result is that it relates chirp , which is measured very accurately, and Λ˜ , which contains important information on the EOS. Hence, when chirp is measured in future detections, our relation can be used to set tight constraints on Λ˜ .
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影响因子：
56.9
作者：
Dietrich, Tim;Coughlin, Michael W.;Antier, Sarah
通讯作者：
Antier, Sarah
DOI：
10.3847/2041-8213/ac089a
发表时间：
2021-05
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
G. Raaijmakers;S. K. Greif;K. Hebeler;T. Hinderer;S. Nissanke;A. Schwenk;T. E. Riley;A. Watts
通讯作者：
G. Raaijmakers;S. K. Greif;K. Hebeler;T. Hinderer;S. Nissanke;A. Schwenk;T. E. Riley;A. Watts
中子星合并状态方程
影响因子：
2.9
作者：
Dexheimer, Veronica;Constantinou, Constantinos;Most, Elias R.;Papenfort, L. Jens;Hanauske, Matthias;Schramm, Stefan;Stoecker, Horst;Rezzolla, Luciano
通讯作者：
Rezzolla, Luciano
DOI：
10.3847/2041-8213/ac03b8
发表时间：
2021-04
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
E. Fonseca;H. Cromartie;T. Pennucci;P. Ray;A. Kirichenko;S. Ransom;P. Demorest;I. Stairs;Z. A
通讯作者：
E. Fonseca;H. Cromartie;T. Pennucci;P. Ray;A. Kirichenko;S. Ransom;P. Demorest;I. Stairs;Z. A
影响因子：
8.7
作者：
Arzoumanian, Zaven;Brazier, Adam;Zhu, Weiwei
通讯作者：
Zhu, Weiwei