Unified Relativistic Mean Field EoSs with density dependent couplings

This dataset, containing 447345 equations of state, was used or the Bayesian analysis on the properties of Neutron Stars in [1]. Each EoS includes an outer crust, an inner crust and a core.The outer crust used for all the EoSs is the BsK22[2], while each pair of inner crust and core was calculatedusing the same Relativistic Mean Field model and a Compressible Liquid Drop approximation for the clusters in the inner crust. The crust-core transition is determined for each model by the crossingof the energy density of crust and core.

[1] L. Scurto, H. Pais and F. Gulminelli, arXiv:2402.15548 (2024)[2] J.M. Pearson, N. Chamel, A.Y. Potekhin, A.F. Fantina, C. Ducoin, A.K. Dutta, and S. Goriely, MNRAS 481, 2994 (2018)

本数据集包含447345个物态方程（Equation of State，下文简称EoS），已被用于文献[1]中针对中子星性质的贝叶斯分析。每个EoS均包含外地壳层、内地壳层与核心区域。所有EoS所采用的外地壳层均为BsK22模型[2]；而每一组内地壳层与核心区域均采用相同的相对论平均场模型（Relativistic Mean Field model），并针对内地壳层中的团簇使用可压缩液滴近似（Compressible Liquid Drop approximation）进行计算。每个模型的壳层-核心相变边界均通过对比地壳与核心的能量密度交点来确定。

[1] L. Scurto, H. Pais and F. Gulminelli, arXiv:2402.15548 (2024)
[2] J.M. Pearson, N. Chamel, A.Y. Potekhin, A.F. Fantina, C. Ducoin, A.K. Dutta, and S. Goriely, MNRAS 481, 2994 (2018)