遍历星模型在参数空间中的定位
Locating ergostar models in parameter space
摘要：
最近，我们证明了具有可压缩因果状态方程的动态稳定的各向异性解（包含一个各向异性区的平衡态中子星）的存在[A. Tsokaros，M.鲁伊斯湖孙习L. Shapiro和K. Uryeland，Phys. Rev. Lett. 123，231103（2019）]。这些恒星是超大质量的，有差异的旋转，并且高度紧凑。本文对平衡态模型进行了系统的研究，以确定各能星在参数空间中的位置。我们采用四个状态方程，不同的匹配密度的最大刚性核心。通过构建大量的模型，均匀和不同程度的微分旋转，我们确定的参数，遍历星出现。我们发现，动态稳定的ergostars出现的最有利条件是一个显着的有限密度接近恒星的表面（即，类似于自束缚夸克星）和小程度的微分旋转。
英文摘要：
Recently, we have shown that dynamically stable ergostar solutions (equilibrium neutron stars that contain an ergoregion) with a compressible and causal equation of state exist [A. Tsokaros, M. Ruiz, L. Sun, S. L. Shapiro, and K. Uryū, Phys. Rev. Lett. 123, 231103 (2019)]. These stars are hypermassive, differentially rotating, and highly compact. In this work, we make a systematic study of equilibrium models in order to locate the position of ergostars in parameter space. We adopt four equations of state that differ in the matching density of a maximally stiff core. By constructing a large number of models both with uniform and differential rotation of different degrees, we identify the parameters for which ergostars appear. We find that the most favorable conditions for the appearance of dynamically stable ergostars are a significant finite density close to the surface of the star (i.e., similar to self-bound quark stars) and a small degree of differential rotation.
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