AI 中文总结
研究温暖磁化恒星物质中轻核团簇相关问题，在广义相对论平均场框架内，考虑磁场与轻核团簇形成相互作用，纳入轻核团簇自由度并描述其溶解，揭示其对物质热力学特性的影响及对称能作用，为相关建模和EOS开发提供见解与基础。
AI 中文摘要
具有成分依赖效应可控处理的有限温度状态方程（EOS），对于模拟原中子星和双中子星合并残骸愈发重要，其中温暖物质可能与强磁场共存。在亚饱和密度下，轻核团簇也可能大量出现。对于β平衡物质，无论有无中微子俘获，磁场与轻核团簇形成之间的相互作用在决定物质组成时自然产生。本文在广义相对论平均场框架内研究这种相互作用，纳入直至α粒子的轻核团簇作为显式自由度，并通过唯象结合能位移描述其在介质中的溶解。研究表明，轻核团簇的形成与溶解，结合磁场效应，在物质压力、等温声速平方和热容量中留下特征印记，显著改变EOS的热力学刚度和温暖恒星物质的蓄热特性。此外，还研究了EOS的同位旋项即对称能对这些特征的影响。这些结果为原中子星和中子星合并残骸的流体动力学和热演化建模提供微观见解，同时为开发更全面的致密星应用有限温度EOS奠定基础。
英文摘要
Finite-temperature equations of state (EOSs) with a controlled treatment of composition-dependent effects are becoming increasingly important for modeling proto-neutron stars and binary neutron star merger remnants, where warm matter may coexist with strong magnetic fields. At sub-saturation densities, light nuclear clusters may also emerge with sizeable abundances. For beta-equilibrated matter, with or without neutrino trapping, an interplay between magnetic fields and light-cluster formation naturally arises in determining the matter composition: charge neutrality and weak equilibrium transmit the effects of Landau quantization to the baryonic sector, modifying the equilibrium charge content; at the same time, light-cluster formation also favors the increase of the proton fraction by binding protons into nuclear clusters. In this work, we investigate this interplay within a generalized relativistic mean-field framework, in which light clusters up to alpha particles are included as explicit degrees of freedom and their in-medium dissolution is described through phenomenological binding-energy shifts. We show that the formation and subsequent dissolution of light clusters, combined with magnetic-field effects, leave characteristic signatures in the matter pressure, the isothermal squared speed of sound, and the heat capacity, leading to significant modifications of the thermodynamic stiffness of the EOS and of the heat-storage properties of warm stellar matter. Furthermore, we investigate the impact of the isovector terms of the EOS, namely its symmetry energy, on these features. These results provide microscopic insights relevant to modeling the hydrodynamic and thermal evolution of proto-neutron stars and neutron star merger remnants, while establishing a baseline for the development of more comprehensive finite-temperature EOSs for compact-star applications.
Comments15 pages, 11 figures
