密集QCD中多重相变对致密恒星的影响

A. Sedrakian
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引用次数: 2

摘要

本文综述了致密QCD物理学的几个最新进展,重点讨论了多相变对致密恒星天体物理表现的影响。为了激发致密量子镉的多相建模和描绘前景,我们首先讨论了其相图的结构以及可能的彩色超导和其他相的排列。推测β平衡的对相关夸克物质与自旋不平衡冷原子和同位旋不对称核物质属于同一普适类。这就意味着具有破缺空间对称性和三临界(Lifshitz)点的相的出现。在考虑间隙函数的频率依赖(延迟)的Eliashberg理论中,讨论了二味夸克和三味夸克物质的夸克传播子的超中场结构及其非平凡意义。然后,我们通过加入声速为cconf的共形流体,构造了一个状态方程(EoS),扩展了密度夸克物质在恒定声速参数化下的两相状态方程。=1/3,密度≥10nsat,其中nsat为饱和密度。有了这个输入,我们在质量半径图中构造了静态的、球对称的致密混合星,恢复了双胞胎和三胞胎等特征,并表明向保形流体的过渡导致了图中轨迹的螺旋入。螺旋上的恒星相对于径向振荡是经典的不稳定的,但如果其界面上夸克相和核子相之间的转换时间尺度大于振荡周期,则可以稳定。最后,我们回顾了从高温间隙到低温无间隙的双味相转变对混合恒星热演化的影响。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Impact of Multiple Phase Transitions in Dense QCD on Compact Stars
This review covers several recent developments in the physics of dense QCD with an emphasis on the impact of multiple phase transitions on astrophysical manifestations of compact stars. To motivate the multi-phase modeling of dense QCD and delineate the perspectives, we start with a discussion of the structure of its phase diagram and the arrangement of possible color-superconducting and other phases. It is conjectured that pair-correlated quark matter in β-equilibrium is within the same universality class as spin-imbalanced cold atoms and the isospin asymmetrical nucleonic matter. This then implies the emergence of phases with broken space symmetries and tri-critical (Lifshitz) points. The beyond-mean-field structure of the quark propagator and its non-trivial implications are discussed in the cases of two- and three-flavor quark matter within the Eliashberg theory, which takes into account the frequency dependence (retardation) of the gap function. We then construct an equation of state (EoS) that extends the two-phase EoS of dense quark matter within the constant speed of sound parameterization by adding a conformal fluid with a speed of sound cconf.=1/3 at densities ≥10nsat, where nsat is the saturation density. With this input, we construct static, spherically symmetrical compact hybrid stars in the mass–radius diagram, recover such features as the twins and triplets, and show that the transition to conformal fluid leads to the spiraling-in of the tracks in this diagram. Stars on the spirals are classically unstable with respect to the radial oscillations but can be stabilized if the conversion timescale between quark and nucleonic phases at their interface is larger than the oscillation period. Finally, we review the impact of a transition from high-temperature gapped to low-temperature gapless two-flavor phase on the thermal evolution of hybrid stars.
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