Abstract Within the minimum model of neutron stars (NS) consisting of neutrons, protons and electrons, a new approach is proposed for inferring the symmetry energy of super-dense neutron-rich nucleonic matter above twice the saturation density ρ 0 of nuclear matter directly from integrating iteratively barotropic pressures in both neutron stars and heavy-ion reactions. Simultaneously, the proton fraction of NSs at β equilibrium is extracted as a function of baryon density from the same procedure. An application of this approach using the NS pressure from GW170817 and the pressure in cold symmetric nuclear matter (SNM) extracted earlier by analyzing nuclear collective flow data in relativistic heavy-ion collisions provides a useful constraining band for the symmetry energy above 2 ρ 0 .

中文翻译：

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中子星和重离子反应中正压压力积分得到的超密富中子物质的对称能

摘要 在由中子、质子和电子组成的中子星（NS）最小模型中，提出了一种新方法，可以直接从核物质饱和密度ρ 0 两倍以上推断出超稠密富中子核子物质的对称能。在中子星和重离子反应中迭代地整合正压压力。同时，在 β 平衡时 NSs 的质子分数作为重子密度的函数从相同的程序中提取。使用来自 GW170817 的 NS 压力和之前通过分析相对论重离子碰撞中的核集体流数据提取的冷对称核物质 (SNM) 中的压力，该方法的应用为高于 2 ρ 0 的对称能量提供了有用的约束带。