We use a Bayesian inference analysis to explore the sensitivity of Taylor expansion parameters of the nuclear equation of state (EOS) to the neutron star dimensionless tidal deformability ($\Lambda$) on 1 to 2 solar masses neutron stars. A global power law dependence between tidal deformability and compactness parameter (M/R) is verified over this mass region. To avoid superfluous correlations between the expansion parameters, we use a correlation-free EOS model based on a recently published meta-modeling approach. We find that assumptions in the prior distribution strongly influence the constraints on $\Lambda$. The $\Lambda$ constraints obtained from the neutron star merger event GW170817 prefer low values of $L_{\mathrm{\text{sym}}}$ and $K_{\mathrm{\text{sym}}}$, for a canonical neutron star with 1.4 solar mass. For neutron star with mass $

中文翻译：

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中子星变形性对状态参数方程的影响

我们使用贝叶斯推断分析来探索状态方程核（EOS）的泰勒展开参数对中子星无量纲潮汐可变形性的敏感性（$\Lambda$）在1至2个太阳质量的中子星上。在该质量区域上，验证了潮汐变形性和密实度参数（M / R）之间的全局幂律相关性。为了避免扩展参数之间多余的相关性，我们基于最近发布的元建模方法使用了无相关性的EOS模型。我们发现，先验分布中的假设极大地影响了对$\Lambda$。的$\Lambda$ 从中子星合并事件GW170817获得的约束倾向于较低的 ${\mathrm{大号}}_{\mathrm{\text{象征}}}$ 和 ${ķ}_{\mathrm{\text{象征}}}$，用于太阳质量为1.4的规范中子星。对于质量为$的中子星