Optimal Neutron-star Mass Ranges to Constrain the Equation of State of Nuclear Matter with Electromagnetic and Gravitational-wave Observations
Optimal Neutron-star Mass Ranges to Constrain the Equation of State of Nuclear Matter with Electromagnetic and Gravitational-wave Observations
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DOI：
10.3847/1538-4357/ab2edd
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发表时间：
2019-05
期刊：
影响因子：
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通讯作者：
L. R. Weih;E. Most;L. Rezzolla
中科院分区：
文献类型：
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作者：
L. R. Weih;E. Most;L. Rezzolla
利用一个非常大的图书馆的物理上合理的状态方程（EOSs）包含超过107个成员，并产生超过109恒星模型，我们进行了调查的影响，通过电磁观测的中子星半径测量可以对EOS的核物质。这样的测量很快就可以从正在进行的中子星星内部成分探测器使命中得到，并将补充地球观测系统在引力波探测方面的限制。由于我们的EOS库的统计范围很大，我们可以获得对通常假设的第一个定量估计，即在测量质量最大的中子星（尽管很罕见）的半径时，EOS的高密度部分受到最好的约束。与此同时，我们发现，半径测量的中子星质量M <$1.7 -1.85 M <$的EOS的低密度部分可以提供最强的约束。最后，我们量化了未来任务的半径测量如何进一步提高我们对核密度下物质状态方程的理解。
Exploiting a very large library of physically plausible equations of state (EOSs) containing more than 107 members and yielding more than 109 stellar models, we conduct a survey of the impact that a neutron-star radius measurement via electromagnetic observations can have on the EOS of nuclear matter. Such measurements are soon to be expected from the ongoing Neutron Star Interior Composition Explorer mission and will complement the constraints on the EOS from gravitational-wave detections. Thanks to the large statistical range of our EOS library, we can obtain a first quantitative estimate of the commonly made assumption that the high-density part of the EOS is best constrained when measuring the radius of the most massive, albeit rare, neutron stars with masses M ≳ 2.1 M⊙. At the same time, we find that radius measurements of neutron stars with masses M ≃ 1.7–1.85 M⊙ can provide the strongest constraints on the low-density part of the EOS. Finally, we quantify how radius measurements by future missions can further improve our understanding of the EOS of matter at nuclear densities.