AI 中文总结
研究中子星中磁化致密核物质的状态方程，在简化的相对论平均场基线内，对比线性QHD - I与非线性GM1模型，发现磁星尺度磁场对核心状态方程影响小，核模型依赖性主导，还通过各向同性化状态方程估计普通TOV序列对磁场的敏感性。
AI 中文摘要
我们在一个刻意简化且内部自洽的相对论平均场（RMF）基线内，研究致密中子星物质对规定磁场强度的静态响应。该模型包括处于β平衡和电荷中性的中子、质子、电子和μ子，通过对带电粒子的朗道量子化纳入均匀外磁场。在零温度下自洽评估状态方程，通过领先阶简并索末菲修正估计适度的有限温度效应。通过无磁化近似中的麦克斯韦贡献纳入磁压力各向异性。此基线旨在在引入额外微观物理或动态磁场演化之前隔离磁场效应的层次结构。我们将用作硬基准的线性QHD - I参数化与更现实的非线性GM1模型进行比较。结果表明，典型磁星尺度的磁场对体核心状态方程产生的变化可忽略不计，而仅当磁场接近强量子化区域时才会出现明显的朗道量子化和压力各向异性效应。QHD - I和GM1之间的比较进一步表明，在此探索的场强范围内，核模型依赖性比静态磁场修正占主导地位。作为一种探索性诊断，我们使用各向同性化的状态方程来估计普通TOV质量 - 半径序列对规定磁场的敏感性。这不应被解释为完全各向异性的磁化星计算。反常磁矩、超子、夸克自由度和动态磁场演化留待未来扩展。
英文摘要
We study the static response of dense neutron-star matter to a prescribed magnetic-field strength within a deliberately minimal and internally consistent relativistic mean-field (RMF) baseline. The model includes neutrons, protons, electrons, and muons in beta equilibrium and charge neutrality, with a uniform external magnetic field incorporated through Landau quantisation of the charged species. The equation of state is evaluated self-consistently at zero temperature, while moderate finite-temperature effects are estimated through leading-order degenerate Sommerfeld corrections. Magnetic pressure anisotropy is included through the Maxwell contribution in the no-magnetisation approximation. The purpose of this baseline is to isolate the hierarchy of magnetic-field effects before introducing additional microphysics or dynamical magnetic-field evolution. We compare the linear QHD-I parameterisation, used as a stiff benchmark, with the nonlinear GM1 model as a more realistic reference. The results show that canonical magnetar-scale fields produce negligible changes in the bulk core equation of state, while visible Landau-quantisation and pressure-anisotropy effects emerge only as the field approaches the strongly quantising regime. The comparison between QHD-I and GM1 further shows that nuclear-model dependence dominates over static magnetic-field corrections up to the field strengths explored here. As an exploratory diagnostic, we use the isotropised equation of state to estimate the sensitivity of ordinary TOV mass--radius sequences to the prescribed magnetic field. This should not be interpreted as a fully anisotropic magnetised-star calculation. Anomalous magnetic moments, hyperons, quark degrees of freedom, and dynamical magnetic-field evolution are left for future extensions.
Comments14 pages, 6 figures, 3 tables
