Equation of State Constraints from Nuclear Physics, Neutron Star Masses, and Future Moment of Inertia Measurements
Equation of State Constraints from Nuclear Physics, Neutron Star Masses, and Future Moment of Inertia Measurements
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DOI：
10.3847/1538-4357/abaf55
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发表时间：
2020-05
期刊：
影响因子：
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通讯作者：
S. K. Greif;K. Hebeler;J. Lattimer;C. Pethick;A. Schwenk
中科院分区：
文献类型：
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作者：
S. K. Greif;K. Hebeler;J. Lattimer;C. Pethick;A. Schwenk
我们探索约束条件的状态方程（EOS）的中子丰富的物质的基础上微观计算核密度和中子星的观测。在以前的工作中，我们表明，预测的基础上，现代核相互作用的手征有效场论和两个太阳质量的中子星的观测结果在一个强大的不确定性范围内的中子星星半径和EOS在很宽的密度范围。在这项工作中，我们扩展了这项研究，采用Hebeler等人的分段多边形扩展以及Greif等人的声速模型，表明中子星转动惯量的测量可以显著改善对物态方程和中子星星半径的约束。
We explore constraints on the equation of state (EOS) of neutron-rich matter based on microscopic calculations up to nuclear densities and observations of neutron stars. In a previous work we showed that predictions based on modern nuclear interactions derived within chiral effective field theory and the observation of two-solar-mass neutron stars result in a robust uncertainty range for neutron star radii and the EOS over a wide range of densities. In this work we extend this study, employing both the piecewise polytrope extension from Hebeler et al. as well as the speed of sound model of Greif et al., and show that moment of inertia measurements of neutron stars can significantly improve the constraints on the EOS and neutron star radii.