With recent advances in neutron star observations, major progress has been made in determining the pressure of neutron star matter at high density. This pressure is constrained by the neutron star deformability, as determined from gravitational waves emitted in a neutron star merger, and measurements of the radii of two neutron stars made using the Neutron Star Interior Composition Explorer X-ray observatory on the International Space Station. Previous studies have relied on nuclear theory calculations to provide the equation of state at low density. Here we use a combination of 15 constraints composed of three astronomical observations and 12 nuclear experimental constraints that extend over a wide range of densities. Bayesian inference is then used to obtain a comprehensive nuclear equation of state. This data-centric result provides benchmarks for theoretical calculations and modelling of nuclear matter and neutron stars. Furthermore, it provides insights into the composition of neutron stars and their cooling due to neutrino radiation.

随着中子星观测的最新进展，在确定高密度中子星物质的压力方面取得了重大进展。这种压力受到中子星变形能力的限制，中子星变形能力是根据中子星合并时发出的引力波以及使用国际空间站上的中子星内部成分探测器 X 射线天文台对两颗中子星的半径进行的测量来确定的。先前的研究依赖于核理论计算来提供低密度下的状态方程。在这里，我们使用了 15 个约束的组合，其中包括三个天文观测和 12 个核实验约束，这些约束延伸到了广泛的密度范围。然后使用贝叶斯推理来获得全面的核状态方程。这一以数据为中心的结果为核物质和中子星的理论计算和建模提供了基准。此外，它还提供了对中子星的组成及其因中微子辐射而冷却的见解。