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GW190814: Impact of a 2.6 solar mass neutron star on the nucleonic equations of state

机译:GW190814:2.6太阳能中子明星对状态核子方程的影响

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Is the secondary component of GW190814 the lightest black hole or the heaviest neutron star ever discovered in a double compact-object system [Abbott et al. Astrophys. J. 896, L44 2020)]? This is the central question animating this paper. 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: (i) account for a 2.6 M-circle dot neutron star, (ii) satisfy the original constraint on the tidal deformability of a 1.4M(circle dot) neutron star, and (iii) 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 supermassive 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 2.6M(circle dot) compact object is likely to be the lightest black hole ever discovered.
机译:GW190814的第二个组成部分是在双致密天体系统中发现的最轻的黑洞还是最重的中子星[Abbott et al.Astrophys.J.896,L44 2020)]?这是本文的核心问题。协变密度泛函理论为研究有限核和中子星的性质提供了一个独特的框架,同时在所有密度下加强了因果关系。通过调整现有的能量密度泛函,我们能够:(i)解释2.6米圆点中子星,(ii)满足1.4米(圆点)中子星潮汐变形能力的原始约束,以及(iii)再现有限核的基态特性。然而,对于这项工作中探索的这类模型,我们发现,支持超大质量中子星所需的状态方程的加强与高能重离子碰撞或中等质量恒星的低变形性所获得的约束不一致。因此,我们推测,中子星的最大质量不能明显高于现有的观测极限,2.6米(圆点)的致密天体可能是迄今为止发现的最轻的黑洞。

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