标题： 基于合并后演化的中子星最大质量约束 显示英文标题

标题： Constraints of the maximum mass of quark stars based on post-merger evolutions

摘要： 我们半解析地研究了双中子星合并后的演化过程。 有效单体方法被用来估计在 inspiral 阶段由于引力波引起的能量和角动量耗散。 在合并后阶段考虑了三种主要的能量和角动量耗散机制：质量外流、中微子和引力波。 每种机制的比例可以通过重子数、能量和角动量守恒定律以及旋转中子星的平衡模型来确定。 将此分析应用于 GW170817 事件得出两个重要结论：1）一个质量小于均匀旋转中子星最大质量的残余中子星可能在其旋转能量通过电磁辐射（即$\sim 100\,\mathrm{s}$）耗散之前发生坍缩，因为残余中子星中剩余的角动量可能不足以维持由于质量外流、中微子和引力波的角动量耗散而增加的超大质量中子星的自引力；2）考虑到一般的中子星状态方程模型，发现了一个关于冷且非旋转中子星最大质量的约束为$M_{\mathrm{TOV}}\lesssim2.35^{+0.07}_{-0.17}\,M_{\odot}$，假设在 GW170817 事件中，在合并残余体的总旋转能量（$\color{blue} \gtrsim 10^{53}\,$erg ）的大部分被沉积到合并环境中之前发生了延迟坍缩。 这些约束可以通过未来的合并事件得到改进，一旦有更多关于其合并后演化通道的证据或来自多信使观测推断的合并后引力波和中微子发射量的信息。 显示英文摘要

摘要： We semi-analytically investigate the post-merger evolution of the binary quark star merger. The effective-one-body method is employed to estimate the energy and angular momentum dissipation due to gravitational waves in the inspiral phase. Three major mechanisms of energy and angular momentum dissipation are considered in the post-merger phase: mass outflows, neutrinos, and gravitational waves. The proportion of each mechanism could be determined by baryon number, energy and angular momentum conservation laws as well as the equilibrium model for rotating quark stars. Applying this analysis to the GW170817 event suggests two important conclusions: 1) a remnant quark star whose mass is smaller than the maximum mass of a uniformly rotating quark star can collapse before its rotational energy is dissipated via electromagnetic radiation (i.e., $\sim 100\,\mathrm{s}$) as the angular momentum left in the remnant quark star might not be large enough to sustain the additional self-gravity of the supramassive quark star due to the angular momentum dissipation of mass outflows, neutrinos and gravitational waves; 2) considering a general quark star equation of state model, a constraint on the maximum mass of cold and non-rotating quark stars is found as $M_{\mathrm{TOV}}\lesssim2.35^{+0.07}_{-0.17}\,M_{\odot}$, assuming a delayed collapse occurred before a large fraction of the total rotational energy ($\color{blue} \gtrsim 10^{53}\,$erg) of the merger remnant was deposited into the merger environment for the GW170817 event. These constraints could be improved with future merger events, once there are more evidences on its post-merger evolution channel or information on the amount of post-merger gravitational wave and neutrino emissions inferred from the multi-messenger observations.