论文标题
通过贝叶斯分析来限制GW170817中子星的核对称能和性能
Constraining the nuclear symmetry energy and properties of neutron star from GW170817 by Bayesian analysis
论文作者
论文摘要
基于潮汐变形的分布和二进制中子星合并GW170817的分量质量，使用状态的参数方程（EOS）用于探测中子星的核对称能和性质。为了获得与观察一致的EOS参数的正确分布，使用贝叶斯分析，并考虑因果关系的约束和最大质量。从该分析中可以发现，核物质的饱和密度可以约束$ e_ {sym}（2 {ρ_{0}}）$ = $ 34.5^{+20.5} _ { - 2.3} $ MEV在90 \％可信度下。此外，还通过此分析证明了对规范中子星的半径和无量纲的潮汐变形的约束，相应的约束为10.80 km $ <r_ {1.4} <$ 13.20 km和$ 133 <λ_{1.4} <λ_{1.4} <686 <686 <686 <686 <686 $ at 90 \％\％\％\％的可靠性水平，是最大的最大值，是最佳的价值，是何种最佳的价值，均有价值，何种; $ \ bar {r} _ {1.4} $ = 12.60 km和$ \barλ_{1.4} $ = 500。关于先验，我们的结果（后结果）更喜欢柔软的EOS，相当于对称能的预期值较低，半径较小和潮汐变形性较小。
Based on the distribution of tidal deformabilities and component masses of binary neutron star merger GW170817, the parametric equation of states (EOS) are employed to probe the nuclear symmetry energy and the properties of neutron star. To obtain a proper distribution of the parameters of the EOS that is consistent with the observation, Bayesian analysis is used and the constraints of causality and maximum mass are considered. From this analysis, it is found that the symmetry energy at twice the saturation density of nuclear matter can be constrained within $E_{sym}(2{ρ_{0}})$ = $34.5^{+20.5}_{-2.3}$ MeV at 90\% credible level. Moreover, the constraints on the radii and dimensionless tidal deformabilities of canonical neutron stars are also demonstrated through this analysis, and the corresponding constraints are 10.80 km $< R_{1.4} <$ 13.20 km and $133 < Λ_{1.4} < 686$ at 90\% credible level, with the most probable value of $\bar{R}_{1.4}$ = 12.60 km and $\barΛ_{1.4}$ = 500, respectively. With respect to the prior, our result (posterior result) prefers a softer EOS, corresponding to a lower expected value of symmetry energy, a smaller radius and a smaller tidal deformability.
