论文标题
贝叶斯方法中对状态密集物质方程的几乎独立的限制
Nearly model-independent constraints on dense matter equation of state in a Bayesian approach
论文作者
论文摘要
我们采用贝叶斯方法来构建大量最小限制的状态方程（EOSS），并研究其与中子星（NS）的一些选定特性的相关性。我们的一组最小约束包括饱和核物质的一些基本特性和低密度纯中子物质EOS，这些特性是从精确的近代到接头到领先阶（n $^{3} $ lo）计算中从手性有效场理论中获得的。发现质量$ 1-2 m_ \ odot $的NS的潮汐变形性和半径与$β$平衡的物质的压力密切相关，高度高于饱和密度（$ρ_0= 0.16 $ fm $^{ - 3} $），几乎是模型依赖性的方式。这些相关性用于$β$平衡物质的压力，约为2 $ρ_0$，是中子星质量和相应的潮汐变形性的函数。还发现中子星的最大质量与$β$平衡物质的压力密切相关。
We apply Bayesian approach to construct a large number of minimally constrained equations of state (EOSs) and study their correlations with a few selected properties of a neutron star (NS). Our set of minimal constraints includes a few basic properties of saturated nuclear matter and low-density pure neutron matter EOS which is obtained from a precise next-to-next-to-next-to-leading-order (N$^{3}$LO) calculation in chiral effective field theory. The tidal deformability and radius of NS with mass $1-2 M_\odot$ are found to be strongly correlated with the pressure of $β$-equilibrated matter at densities higher than the saturation density ($ρ_0 = 0.16$ fm$^{-3}$) in a nearly model-independent manner. These correlations are employed to parametrize the pressure for $β$-equilibrated matter, around 2$ρ_0$, as a function of neutron star mass and the corresponding tidal deformability. The maximum mass of neutron star is also found to be strongly correlated with the pressure of $β$-equilibrated matter at densities $\sim 4.5ρ_0$.
