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arXiv 2001.06294nucl-thgr-qc
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从微观核动力学模型研究中子星的潮汐形变

Tidal Deformation of Neutron Stars from Microscopic Models of Nuclear Dynamics

Andrea Sabatucci, Omar Benhar

备注：
Accepted for publication in Physical Review C
发表信息：
Phys. Rev. C 101, 045807 (2020)
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摘要：

观测到的引力波信号GW 170817与一个中子星双星系统螺旋内的辐射一致，提供了有关参与恒星潮汐变形的信息。现有的数据可以用来约束致密核物质的状态方程，以及揭示在微观水平上描述核动力学的基础模型。在本文中，我们比较实验结果的预测不同的理论模型，基于非相对论性核多体理论，相对论性场论的形式主义，和更多的唯象方法所观察到的核性质的约束。虽然现有数据的精度不允许解决模型的简并性，但我们的分析显示出对不同状态方程预测的恒星紧凑性的明显敏感性，这被证明是对核子-核子势的相对论增强修正的显著影响。

英文摘要：

The observation of the gravitational wave signal GW170817, consistent with emission from the inspiral of a binary neutron-star system, provided information on the tidal deformation of the participating stars. The available data may be exploited to constrain the equation of state of densenuclear matter, as well as to shed light on the underlying models describing nuclear dynamics at microscopic level. In this paper we compare the experimental results to the predictions of different theoretical models, based on non relativistic nuclear many-body theory, the relativistic field-theoretical formalism, and a more phenomenological approach constrained by observed nuclear properties. While the precision of the available data does not allow to resolve the degeneracy of the models, our analysis shows a distinct sensitivity to the star compactness predicted by the different equations of state, which turns out to be significantly affected by relativistic boost corrections to the nucleon-nucleon potential.

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