AI 中文总结
研究中子星冷却特性，聚焦有效核子质量，采用瓦莱卡模型及基于相对论平均场理论的状态方程进行冷却模拟，发现狄拉克和朗道质量影响大质量中子星冷却，有效核子质量处理或为冷却不确定性重要来源。
AI 中文摘要
由超高密度核物质组成的中子星冷却强烈依赖于状态方程，因为主要冷却源是其内部产生的中微子。我们研究中子星的冷却特性，聚焦于有效核子质量，其影响最近在超新星爆炸和原中子星冷却中被研究。有效质量的不确定性源于标量介子吸引相互作用的差异以及狄拉克质量和朗道质量的定义。首先采用瓦莱卡模型在统一框架内引入这两种质量并评估冷却曲线，基于此计算中子发射率、直接乌卡过程及其冷却曲线。结果表明狄拉克质量和朗道质量影响大质量中子星冷却，此前多数冷却模拟未区分它们。还用基于相对论平均场理论的两种现实状态方程进行冷却模拟，结果与瓦莱卡模型大致一致，表明有效核子质量的处理可能是中子星冷却不确定性的重要来源。
英文摘要
The cooling of neutrons stars, which are composed of ultra-high-density nuclear matter, strongly depends on the equation of state because the dominant cooling sources are neutrinos produced in their interiors. Here, we investigate the cooling properties of neutron stars, focusing on effective nucleon masses, whose impacts have been recently examined in supernova explosion and proto-neutron star cooling. The uncertainties of effective masses originate from the difference in the attractive interaction of scalar meson and the definition of the Dirac and Landau masses. At first, we employ so-called Walecka models that allow these two masses to be introduced within a unified framework and evaluate the resulting cooling curves. Based on the Walecka model, we compute the emissivity of the neutrons and the direct Urca process and their cooling curves. We demonstrate that the Dirac and Landau masses affect cooling of massive neutron stars, although most previous cooling simulations do not distinguish them. We also perform cooling simulations with two realistic equation of states based on relativistic mean-field (RMF) theory, whose differences arise from properties of only effective masses among characteristic parameters. These results are broadly consistent with those obtained from the Walecka models, indicating that the treatment of effective nucleon masses may be an important source of uncertainty in neutron-star cooling.
Comments17 pages, 5 figures
