论文标题
GW190814：2.6太阳质量中子星对状态核方程的影响
GW190814: Impact of a 2.6 solar mass neutron star on nucleonic equations of state
论文作者
论文摘要
是GW190814的次要组成部分，是最轻的黑洞或有史以来最重的中子星在双重紧凑型对象系统中[R. R. Abbott等人，APJ Lett。，896，L44（2020）]？这是动画这封信的核心问题。协变密度功能理论提供了一个独特的框架，以研究有限核和中子星的性质，同时在所有密度下都强化因果关系。通过调整现有的能量密度函数，我们能够：（a）考虑2.6 MSUN中子星，（b）满足1.4 MSUN Neutron Star的潮汐变形性的原始约束，以及（c）繁殖有限核的地面特性。然而，对于这项工作中探索的模型类别，我们发现支持超质量中子星的状态方程的僵硬与从能量重型离子碰撞或中等质量恒星的低变形性获得的约束不一致。因此，我们推测最大的中子星质量不能显着高于现有的观察限制，并且2.6 MSUN紧凑型物体可能是有史以来最浅的黑洞。
Is the secondary component of GW190814 the lightest black hole or the heaviest neutron star ever discovered in a double compact-object system [R. Abbott et al., ApJ Lett., 896, L44 (2020)]? This is the central question animating this letter. Covariant density functional theory provides a unique framework to investigate both the properties of finite nuclei and neutron stars, while enforcing causality at all densities. By tuning existing energy density functionals we were able to: (a) account for a 2.6 Msun neutron star, (b) satisfy the original constraint on the tidal deformability of a 1.4 Msun neutron star, and (c) reproduce ground-state properties of finite nuclei. Yet, for the class of models explored in this work, we find that the stiffening of the equation of state required to support super-massive neutron stars is inconsistent with either constraints obtained from energetic heavy-ion collisions or from the low deformability of medium-mass stars. Thus, we speculate that the maximum neutron star mass can not be significantly higher than the existing observational limit and that the 2.6 Msun compact object is likely to be the lightest black hole ever discovered.
