标题： 从双中子星并合的引力波辐射中推断合并后的引力波发射 显示英文标题

标题： Inferring the post-merger gravitational wave emission from binary neutron star coalescences

摘要： 我们提出了一种稳健的方法，用于表征中子星合并残余体的引力波辐射。 我们的方法对信号的形态做出了最少的假设，并提供了潜在波形的完整后验概率分布。 我们将该方法应用于先进地面探测器网络的模拟数据，并展示了引力波信号的重建。 我们研究了不同双星配置和碰撞中子星的状态方程对重建质量的影响。 我们展示了如何利用该方法来限制尚不确定的中子星物质状态方程。 我们得出的状态方程约束与在后期 inspiral 阶段对碰撞中子星潮汐变形的测量结果相辅相成。 在双中子星 inspiral 后未检测到合并后信号的情况下，我们能够对发射的能量设定上限。 显示英文摘要

摘要： We present a robust method to characterize the gravitational wave emission from the remnant of a neutron star coalescence. Our approach makes only minimal assumptions about the morphology of the signal and provides a full posterior probability distribution of the underlying waveform. We apply our method on simulated data from a network of advanced ground-based detectors and demonstrate the gravitational wave signal reconstruction. We study the reconstruction quality for different binary configurations and equations of state for the colliding neutron stars. We show how our method can be used to constrain the yet-uncertain equation of state of neutron star matter. The constraints on the equation of state we derive are complimentary to measurements of the tidal deformation of the colliding neutron stars during the late inspiral phase. In the case of a non-detection of a post-merger signal following a binary neutron star inspiral we show that we can place upper limits on the energy emitted.