Although the main features of the evolution of binary neutron star systems are now well established, many details are still subject to debate, especially regarding the post-merger phase. In particular, the lifetime of the hyper-massive neutron stars formed after the merger is very hard to predict. In this work, we provide a simple analytic relation for the lifetime of the merger remnant as function of the initial mass of the neutron stars. This relation results from a joint fit of data from observational evidence and from various numerical simulations. In this way, a large range of collapse times, physical effects and equation of states is covered. Finally, we apply the relation to the gravitational wave event GW170817 to constrain the equation of state of dense matter.

尽管现在已经很好地确定了双星中子星系统演化的主要特征，但是许多细节仍在争论中，尤其是在合并后阶段。特别是，合并后形成的超大质量中子星的寿命很难预测。在这项工作中，我们提供了合并残余物的寿命与中子星初始质量的函数的简单解析关系。这种关系是来自观察证据和各种数值模拟的联合数据拟合得出的。这样，涵盖了大范围的坍塌时间，物理效应和状态方程。最后，我们将该关系应用于引力波事件GW170817，以约束致密物的状态方程。