论文标题
核能密度函数的状态和潮汐变形性的中子星方程
Neutron star equation of state and tidal deformability with nuclear energy density functionals
论文作者
论文摘要
中子恒星是致密核物质物理学的最终测试场所。在从二元中子星的合并中检测引力波之前，已经使用各种状态核方程来估计基于电磁观测值的中子恒星（例如质量和半径）的宏观特性。然而，最近对引力波GW170817的中子星的潮汐变形性的观察开辟了一个新时代的多门神天文学和天体物理学，并且已经扩展了许多理论作品以估计中子星的潮汐变形性。在本文中，我们回顾了有关核能密度函数应用于中子恒星特性（包括潮汐变形性）的最新著作。我们发现许多核能密度功能，包括新的孩子（韩国：IBS-DAEGU-SUNGKYUNKWAN）模型，都满足了当前电磁和引力波观测的两种约束。我们讨论了从基于地面实验和多理智观察结果中限制状态核物质方程的未来可能性。
Neutron star is the ultimate testing place for the physics of dense nuclear matter. Before the detection of gravitational waves from the merger of binary neutron stars, various nuclear equations of state have been used to estimate the macroscopic properties of neutron stars, such as masses and radii, based on the electromagnetic observations. However, recent observations on the tidal deformability of neutron star from the gravitational waves GW170817 opened a new era of multi-messenger astronomy and astrophysics, and many theoretical works have been extended to estimate the tidal deformability of neutron stars. In this article, we review our recent works on the application of nuclear energy density functionals to the properties of neutron stars including tidal deformability. We found that many nuclear energy density functionals, including new KIDS (Korea: IBS-Daegu-Sungkyunkwan) model, satisfy both constraints from current electromagnetic and gravitational wave observations. We discuss future possibilities of constraining nuclear matter equation of state from ground-based experiments and multi-messenger observations.
