arXivDaily arXiv每日学术速递 周一至周五更新
arXiv 2408.01302nucl-thhep-ph
收藏

宇称双重态模型的热力学:非对称物质与中子物质

Thermodynamics of the parity-doublet model: Asymmetric and neutron matter

Jürgen Eser, Jean-Paul Blaizot

AI总结:

本文在宇称双重态模型中研究同位旋非对称物质至纯中子物质的热力学相结构,通过将间隙方程化为常微分方程求解自由能,揭示手征伙伴占据阈值由费米子参数决定,并计算中子物质状态方程与声速以对比中子星观测。

摘要:

我们在扩展平均场计算中考虑宇称双重态模型内的同位旋非对称物质,将中子过剩连续增加直至纯中子物质。我们计算了从零到中等温度下发生的液-气相变和手征相变,但特别强调零温度和大重子密度下物质的相结构。自由能的计算涉及间隙方程的求解。这是通过将这些间隙方程变换为控制各种物理量随重子密度增加而流动的常微分方程来实现的:同位旋标量凝聚、质子与中子的密度,以及它们各自手征伙伴的密度。在这一表述中,微分方程的初始条件决定了整个相结构。进一步证明,手征伙伴粒子开始占据的阈值完全由费米子参数决定,最显著的是由核子的手征不变质量决定。我们强调了宇称对称能在驱动核子及其宇称伙伴跨越手征相变达到平衡中的作用。我们详细分析了随着中子过剩的变化物质性质的变化,包括对手征极限的专门讨论,并系统地将宇称双重态模型与其对应的单态模型进行比较,后者忽略了核子的手征伙伴。最后,我们聚焦于中子物质,计算了状态方程和声速。结果与其他计算以及近期对中子星观测的贝叶斯分析进行了对比。

英文摘要:

We consider isospin-asymmetric matter in the parity-doublet model within an extended mean-field calculation, increasing continuously the neutron excess all the way to pure neutron matter. We compute the liquid-gas and the chiral phase transitions occurring at zero to moderate temperatures, but put special emphasis on the phase structure of matter at zero temperature and large baryon densities. The calculation of the free energy involves the solution of gap equations. This is achieved by transforming these gap equations into ordinary differential equations that control the flow with increasing baryon density of various physical quantities: the isoscalar condensate, the densities of protons and neutrons, as well as those of their respective chiral partners. In this formulation, the initial conditions for the differential equations determine the entire phase structure. It is further demonstrated that the threshold for the onset of the population of the chiral partners is exclusively determined by the fermionic parameters, most notably by the chiral-invariant mass of the nucleon. We underline the role of a parity symmetry energy in driving the equilibration of the nucleons and their parity partners across the chiral transition. We provide a detailed analysis of the changes in the matter properties as one varies the neutron excess, including a special discussion of the chiral limit, and we compare systematically the parity-doublet model to its corresponding singlet model, where the chiral partner of the nucleon is neglected. Finally, we focus on neutron matter and compute the equation of state and the speed of sound. The results are confronted to those of other calculations as well as to recent Bayesian analyses of neutron-star observations.

机构、总结、中文摘要均由AI分析而来,可能存在错误,请以论文正文为准。

↑