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经验中子星质量方程在约束核物质状态方程参数中的应用

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联合多种数据已成为约束核物质状态方程的有效方法之一。中子星的经验质量方程提供了天体观测量与地面实验室观测量之间的关联，为相关研究提供了便利的基础。本文基于208Pb的中子皮厚度和偶极极化率的实验数据，在中子星模型和贝叶斯统计方法的理论框架下，计算了核物质状态方程参数、中子星半径、中子星潮汐形变系数以及中子星引力红移的后验概率分布。研究结果显示，中子星的经验质量方程在约束核物质状态方程方面具有显著效果。中子皮厚度数据能够提供与中子星半径观测数据相媲美的约束效果。基于PREX-Ⅱ合作组发布的中子皮厚度数据，中子星经验质量方程对应更硬的核物质状态方程。通过计算1。4倍太阳质量中子星引力红移的后验概率分布，发现源GS1826-24的质量有较大概率为1。4倍太阳质量。结合中子星半径观测和208Pb的中子皮厚度与偶极极化率的联合数据，发现相对于中子皮厚度数据，中子星半径和偶极极化率数据在约束核物质状态方程参数方面起着更为重要的作用。208Pb的偶极极化率数据表现出最佳的约束效果，突显了在解决核物质状态方程这一复杂问题中实验数据的丰富性和精确性的重要性。
Implications of the empirical neutron-star mass formula in constraining the parameters of the nuclear equation of state
The integration of multiple datasets has emerged as an effective method for constraining the equation of state of nuclear matter.The empirical mass formula of neutron stars establishes a correlation between astrophysical and ground-based laboratory observations,providing a convenient framework for related investigations.In this study,based on experimental data of the neutron skin thickness and dipole polarizability of 208Pb,we estimate the posterior probability distributions of the parameters of the equation of state of nuclear matter,neutron star radius,tidal deformability,and gravitational redshift within the theoretical framework of neutron star models and Bayesian statistical methods.The results show that the empirical mass formula of neutron stars considerably influences the constraint of the equation of state of nuclear matter.The neutron skin thickness data exhibit a comparable constraining effect to neutron star radius observations.Based on the neutron skin thickness data released by the PREX-Ⅱ Collaboration,the empirical mass formula supports a stiffer equation of state for nuclear matter than these from the neutron star radius observations.By calculating the posterior probability distribution of the gravitational redshift for a normal neutron star,there is a substantial likelihood that the mass of the source GS1826-24 is found to be approximately 1.4 times the solar mass.Combining neutron star radius observations with the joint data of the neutron skin thickness and dipole polarizability of 208Pb,it is evident that,neutron star radius and dipole polarizability data play a more crucial role than neutron skin thickness data,in constraining the parameters of the equation of state of nuclear matter.The dipole polarizability data of 208Pb demonstrate the most optimal constraint effect,highlighting the significance of rich and precise experimental data in addressing the intricate problem of the equation of state of nuclear matter.

equation of state of nuclear matterBayesian inference approachempirical mass formula of neutron starsneutron skin thicknessdipole polarizability

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运城学院物理与电子工程系,运城 044000

核物质状态方程参数 贝叶斯统计方法 中子星经验质量方程 208Pb的中子皮厚度 208Pb的偶极极化率

山西省基础研究计划山西省留学人员科技活动择优项目运城学院学科建设项目资助

2021030212308520220037

2024

10.1360/SSPMA-2023-0405

中国科学(物理学 力学 天文学)
中国科学院

中国科学(物理学 力学 天文学)

CSTPCD北大核心
影响因子：0.644
ISSN：1674-7275
年,卷(期)：2024.54(6)