论文标题
在相对论的平均场模型中，具有小半径的巨大中子星形恒星优化为核接地状态
Massive neutron stars with small radii in relativistic mean-field models optimized to nuclear ground states
论文作者
论文摘要
我们使用相对论均值场模型具有等轴和等轴 - 膜混合的相对论均值场模型，为中子恒星提供了一个状态方程（EOS）。考虑到中性皮肤厚度的结果，$ r _ {\ rm skin} $，$^{208} $ pb由Prex协作报告的，从GW170817中观察到的规范中性星的无尺度潮汐变形性，以及$ 2.6 $ $ _ $ _ {构建了一种新的有效相互作用，以重现有限的，封闭壳核的核物质和地面特性。我们发现，中子星EOS在核饱和密度的两倍上表现出了快速僵硬，这是由软核对称能引起的，$ e _ {\ rm sym} $。同样值得注意的是，可以通过$ e _ {\ rm sym} $的小斜率参数来实现Prex-2实验的厚$ r _ {\ rm skin} $。因此，我们推测GW190814的次要组件是有史以来最重的中子星。
We present an equation of state (EoS) for neutron stars using the relativistic mean-field model with isoscalar- and isovector-meson mixing. Taking into account the results of the neutron skin thickness, $R_{\rm skin}$, of $^{208}$Pb reported by the PREX collaboration, the dimensionless tidal deformability of a canonical neutron star observed from GW170817, and a $2.6$ $M_{\odot}$ compact star implied by the secondary component of GW190814, a new effective interaction is constructed so as to reproduce the saturation condition of nuclear matter and the ground-state properties of finite, closed-shell nuclei. We find that the neutron star EoS exhibits the rapid stiffening around twice the nuclear saturation density, which is caused by the soft nuclear symmetry energy, $E_{\rm sym}$. It is also noticeable that the thick $R_{\rm skin}$ from the PREX-2 experiment can be achieved with the small slope parameter of $E_{\rm sym}$ stemming from the isoscalar-meson mixing. Thus, we speculate that the secondary component of GW190814 is the heaviest neutron star ever discovered.
