标题： 中子星物质的状态方程，以及核对称性能量 显示英文标题

标题： Equation of state of the neutron star matter, and the nuclear symmetry energy

摘要： 核平均场势能是通过哈特里-福克方法使用不同的介质中核子-核子（NN）相互作用来研究中子星（NS）物质的状态方程（EOS）的。 在零温度下，均匀NS核心的EOS已经计算出来，对于np$e\mu$成分，在$\beta$平衡条件下，使用Skyrme相互作用的版本Sly4以及两种密度依赖的有限范围M3Y相互作用版本（CDM3Y$n$和 M3Y-P$n$），以及Gogny相互作用的版本D1S和D1N。 尽管所考虑的有效NN相互作用在许多核结构和/或反应研究中已被证明非常现实，但它们在超核密度下对核物质对称性能量的行为给出了相当不同的结果，这导致了文献中最近讨论的\emph{软}和\emph{刚性}场景。 中子星核心的不同EOS以及由可压缩液滴模型给出的中子星外壳的EOS被用作托尔曼-奥本海默-沃尔科夫方程的输入，以研究核对称性能量如何影响不同中子星性质的模型预测，如冷却过程以及引力质量、半径和转动惯量。 显示英文摘要

摘要： The nuclear mean-field potentials obtained in the Hartree-Fock method with different choices of the in-medium nucleon-nucleon (NN) interaction have been used to study the equation of state (EOS) of the neutron star (NS) matter. The EOS of the uniform NS core has been calculated for the np$e\mu$ composition in the $\beta$-equilibrium at zero temperature, using version Sly4 of the Skyrme interaction as well as two density-dependent versions of the finite-range M3Y interaction (CDM3Y$n$ and M3Y-P$n$), and versions D1S and D1N of the Gogny interaction. Although the considered effective NN interactions were proven to be quite realistic in numerous nuclear structure and/or reaction studies, they give quite different behaviors of the symmetry energy of nuclear matter at supranuclear densities that lead to the \emph{soft} and \emph{stiff} scenarios discussed recently in the literature. Different EOS's of the NS core and the EOS of the NS crust given by the compressible liquid drop model have been used as input of the Tolman-Oppenheimer-Volkov equations to study how the nuclear symmetry energy affects the model prediction of different NS properties, like the cooling process as well as the gravitational mass, radius, and moment of inertia.