论文标题
具有参数化状态方程的中子星特性的贝叶斯分析：可能性函数的作用
Bayesian analysis of neutron-star properties with parameterized equations of state: the role of the likelihood functions
论文作者
论文摘要
我们研究了采用可变或恒定型函数的中子恒星方程进行贝叶斯推进分析时引入的系统差异。前者的优势是保留有关测量分布的完整信息，从而详尽地使用了数据。另一方面，后者具有更简单的实施和降低计算成本的优势。在这两种方法中，EOSS都具有相同的先验，并且是使用声速参数化方法构建的，以满足X射线和重力波观测的约束，以及手性有效理论和扰动QCD的约束。在所有情况下，这两种方法都会带来非常相似的结果，而$ 90 \％$ - 置信度基本上是重叠的。确实出现了一些差异，但是在概率密度非常小的区域中，主要是由于二进制潮汐变形性$ \tildeλ\ leq 720 $ a the the the the the the fonstant-likelihoodhoodhoodhoodhoodhoodhoodhoodhoodhoodhoodhoodhoodhoodhood ance而言。我们的分析还产生了两个结果。首先，最大巨大恒星的归一化中心数密度，$ n _ {\ rm c，tov}/n_s $与最大巨大恒星的半径，$ r _ {\ rm tov} $之间存在明显的逆相关。其次，最重要的是，它已经确认了chirp质量$ \ Mathcal {m} _ {\ rm chirp} $与二进制潮汐变形$ \tildeλ$之间的关系。此结果的重要性是它关联了一个非常准确测量的数量，$ \ nathcal {m} _ {\ rm chirp} $与包含有关微物理学的重要信息，$ \tildeλ$。因此，一旦$ \ Mathcal {M} _ {\ rm chirp} $在将来的检测中测量，我们的关系就有可能对$ \tildeλ$设置紧密约束。
We have investigated the systematic differences introduced when performing a Bayesian-inference analysis of the equation of state of neutron stars employing either variable- or constant-likelihood functions. The former have the advantage that it retains the full information on the distributions of the measurements, making an exhaustive usage of the data. The latter, on the other hand, have the advantage of a much simpler implementation and reduced computational costs. In both approaches, the EOSs have identical priors and have been built using the sound-speed parameterization method so as to satisfy the constraints from X-ray and gravitational-waves observations, as well as those from Chiral Effective Theory and perturbative QCD. In all cases, the two approaches lead to very similar results and the $90\%$-confidence levels are essentially overlapping. Some differences do appear, but in regions where the probability density is extremely small and are mostly due to the sharp cutoff set on the binary tidal deformability $\tilde Λ\leq 720$ employed in the constant-likelihood analysis. Our analysis has also produced two additional results. First, a clear inverse correlation between the normalized central number density of a maximally massive star, $n_{\rm c, TOV}/n_s$, and the radius of a maximally massive star, $R_{\rm TOV}$. Second, and most importantly, it has confirmed the relation between the chirp mass $\mathcal{M}_{\rm chirp}$ and the binary tidal deformability $\tildeΛ$. The importance of this result is that it relates a quantity that is measured very accurately, $\mathcal{M}_{\rm chirp}$, with a quantity that contains important information on the micro-physics, $\tildeΛ$. Hence, once $\mathcal{M}_{\rm chirp}$ is measured in future detections, our relation has the potential of setting tight constraints on $\tildeΛ$.
