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Constraining the relativistic mean-field model equations of state with gravitational wave observations

机译：用引力波观察约束状态的相对论平均场模型方程

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The first detection of gravitational waves from the binary neutron star merger event GW170817 has started to provide important new constraints on the nuclear equation of state at high density. The tidal deformability bound of GW170817 combined with the observed two solar mass neutron star poses a serious challenge to theoretical formulations of realistic equations of state. We analyze a fully comprehensive set of relativistic nuclear mean-field theories by confronting them with the observational bounds and the measured neutron-skin thickness. We find that only a few models can withstand these bounds which predict a stiff overall equation of state but with a soft neutron-proton symmetry energy. Two possible indications are proposed: Circumstantial evidence of hadron-quark phase transition inside the star and new parametrizations that are consistent with ground-state properties of finite nuclei and observational bounds. Based on extensive analysis of these sets, an upper limit on the radius of a 1.4M(circle dot) neutron star of R-1.4 less than or similar to 12.9 km is deduced.
机译：第一检测来自二元中子星合并事件GW170817的重力波已经开始在高密度下对状态的核方程提供重要的新约束。 GW170817的潮汐可变形性与观察到的两个太阳能中子星结合的界限构成了对州立现实方程式的理论配方的严重挑战。通过将它们与观测范围构成和测量的中子厚度将它们分析了一套全面的相对论核平均场理论。我们发现只有少数型号可以承受这些界限，这些界限预测了刚的整体方程，但具有柔软的中子质对称能量。提出了两种可能的适应症：星形和新的参数化的哈龙夸克阶段过渡的间接证据，这些参数化与有限核和观察范围的地面性质一致。基于对这些集合的广泛分析，推导出1.4米（圆点）中子星的半径的上限，R-1.4小于或类似于12.9公里。

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