论文标题
中子星形可变形性对状态参数方程的影响
Impact of the neutron-star deformability on equation of state parameters
论文作者
论文摘要
我们使用贝叶斯推理分析来探索泰勒膨胀参数（EOS）对1至2个太阳质量中子恒星中Neutron Star的无量纲潮汐变形性（$λ$）的灵敏度。在该质量区域，验证了潮汐变形性和紧凑性参数（M/R）之间的全球功率定律依赖性。为了避免扩展参数之间的多余相关性，我们基于最近发布的元模型方法使用无关联的EOS模型。我们发现，先前分布中的假设强烈影响$λ$的约束。从中子星合并事件GW170817获得的$λ$约束更喜欢$ l_ \ text {sym} $和$ k_ \ text {sym} $的低值，对于具有1.4太阳能质量的规范中子星。对于具有质量$ <1.6 $太阳质量的中子星，$ l_ \ text {sym} $和$ k_ \ text {sym} $与潮汐变形性高度相关。对于更大的中子星，潮汐变形性与高阶泰勒膨胀参数更加密切相关。
We use a Bayesian inference analysis to explore the sensitivity of Taylor expansion parameters of the nuclear equation of state (EOS) to the neutron star dimensionless tidal deformability ($Λ$) 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 $Λ$. The $Λ$ constraints obtained from the neutron star merger event GW170817 prefer low values of $L_\text{sym}$ and $K_\text{sym}$, for a canonical neutron star with 1.4 solar mass. For neutron star with mass $<1.6$ solar mass, $L_\text{sym}$ and $K_\text{sym}$ are highly correlated with the tidal deformability. For more massive neutron stars, the tidal deformability is more strongly correlated with higher order Taylor expansion parameters.
