论文标题
来自瞬态中子恒星F模式振荡的重力波
Gravitational waves from transient neutron star f-mode oscillations
论文作者
论文摘要
在最新的观察过程中，Ligo/处女座报道了重力波（GW）瞬态S191110AF，爆发信号的频率为1.78 kHz，持续了0.104 s。尽管该信号后来被认为是非没应物理的，但将来会出现对不确定起源的真正检测。在这里，我们研究了从中子恒星流体振荡中检测GW的潜力，中子恒星流体振荡的模式频率和持续时间与S191110AF相匹配，并且可用于约束核物质状态的方程。假设这种瞬态振荡可以激发到脉冲星故障的典型能量，我们使用已知的小故障脉冲星的测量特性来估计此类事件产生的GWS的幅度。我们发现，当前的GW探测器可能会观察到附近的脉冲星经历了大型事件，其能量类似于Vela Pulsar Glitch Energies，而下一代探测器可以观察到大量事件。最后，我们表明可以区分通过迅速旋转和缓慢旋转的脉冲星与F模式频率旋转的烙印所产生的GW。
During their most recent observing run, LIGO/Virgo reported the gravitational wave (GW) transient S191110af, a burst signal at a frequency of 1.78 kHz that lasted for 0.104 s. While this signal was later deemed non-astrophysical, genuine detections of uncertain origin will occur in the future. Here we study the potential for detecting GWs from neutron star fluid oscillations, which have mode frequency and duration matching those of S191110af and which can be used to constrain the equation of state of nuclear matter. Assuming that such transient oscillations can be excited to energies typical of a pulsar glitch, we use measured properties of known glitching pulsars to estimate the amplitude of GWs produced by such events. We find that current GW detectors may observe nearby pulsars undergoing large events with energy similar to Vela pulsar glitch energies, while next generation detectors could observe a significant number of events. Finally, we show that it is possible to distinguish between GWs produced by rapidly rotating and slowly rotating pulsars from the imprint of rotation on the f-mode frequency.
