发表机构
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences; School of Astronomy and Space Science, University of Science and Technology of China（中国科学院紫金山天文台暗物质与空间天文重点实验室; 中国科学技术大学天文与空间科学学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用扩充样本和QCD约束，更新了GW170817并合后引力波能量（约0.051太阳质量能量）及中子星最大质量（约2.09-2.18太阳质量）的估计，验证了不同方法的一致性。
AI 中文摘要
在这项工作中，得益于具有测量质量和半径的中子星样本的增加，以及手征有效场论和微扰QCD约束的纳入，对于GW170817中涉及的双中子星，潮汐参数$\kappa_2^T$被约束为$78^{+17}_{-11}$（68.3%置信区间，除非特别说明，本文主要采用此区间）。这样的$\kappa_2^T$有利于并合后阶段的强引力波辐射，相应的能量估计为$E_{\rm GW,p} \simeq 0.051^{+0.022}_{-0.017}\\,M_\odot c^2$。假设双中子星并合后的残骸是一个超质量中子星（正如GW170817电磁对应体的建模所暗示的那样），我们在考虑残骸寿命（$t_{\rm c}$）不确定性的情况下，检验了非旋转中子星的最大质量（$M_{\rm TOV}$）。我们的结果表明，$M_{\rm TOV}$从$t_{\rm c}=0.1$秒时的$2.09^{+0.11}_{-0.09}\\,M_\odot$变化到$t_{\rm c}=1$秒时的$2.18^{+0.10}_{-0.09}\\,M_\odot$。这一结果与独立地从中子星物质状态方程重建中推断出的结果一致，即$M_{\rm TOV,exc}=2.16^{+0.10}_{-0.07}M_\odot$，特别是如果在构建$M_{\rm TOV}$的先验分布时已移除了质量间接测量的非常重的中子星。不同方法发现的非旋转中子星最大质量的一致性表明，我们对这一致密物质物理的关键参数有了合理的理解。
英文摘要
In this work, benefiting from the increased sample of neutron stars with measured masses and radii as well as the incorporation of the chiral effective field theory and perturbative QCD constraints, the tidal parameter $κ_2^T$ is constrained to be $78^{+17}_{-11}$ (68.3% credible interval, mainly adopted in this work unless mentioned specifically) for the binary neutron stars involved in GW170817. Such a $κ_2^T$ is in favor of strong gravitational wave radiation in the post-merger phase and the corresponding energy is estimated to be $E_{\rm GW,p} \simeq 0.051^{+0.022}_{-0.017}\,M_\odot c^2$. Assuming the remnant from binary neutron star merger is a supramassive neutron star, as suggested by the modeling of the electromagnetic counterparts of GW170817, we examine the maximum mass of nonrotating neutron stars ($M_{\rm TOV}$) while accounting for the uncertainty in the remnant's lifetime ($t_{\rm c}$). Our results show that $M_{\rm TOV}$ varies from $2.09^{+0.11}_{-0.09}\,M_\odot$ for $t_{\rm c}=0.1$ s to $2.18^{+0.10}_{-0.09}\,M_\odot$ for $t_{\rm c}=1$ s. This result is consistent with that independently inferred from the re-construction of the equation of state of neutron star matter, i.e., $M_{\rm TOV,exc}=2.16^{+0.10}_{-0.07}M_\odot$, particularly if the very massive neutron stars with masses measured indirectly have been removed in constructing the prior distribution of $M_{\rm TOV}$. The consistency of the maximum mass of nonrotating neutron stars found in different approaches suggests a reasonable understanding of this key parameter for dense-matter physics.
Comments12 pages, 7 figures, ApJ published
Journal ref2026, ApJ, 1008, 114
