论文标题
重力波形模型基于旋转黑洞的光子运动
Gravitational waveform model based on photon motion for spinning black holes
论文作者
论文摘要
来自二进制黑洞合并的波形包括Inspiral，合并和RINDDOWN零件。通常，可以通过从牛顿后近似校准来获得灵感波形。通过黑洞扰动理论，可以从准模式中获得合并和响声。但是，对于更一般的黑洞，准模式的计算不是微不足道的。在本文中，我们使用光子球来获得旋转黑洞的准模式。然后，我们将Ringdown Wave与灵感部件连接起来，以获取完整的波形，并与数值相对性的波形进行比较。我们发现它们彼此非常吻合。原则上，该方法可以扩展到某些一般紧凑的对象。例如，获得了来自参数化轴对称黑洞的环形波形。我们还使用这种方法来获取加速最终黑洞的响声信号；这是由于合并期间重力后坐力造成的。即使在极端情况下，由于后坐力引起的加速度也无法产生可检测的效果。
The waveforms from binary black hole mergers include inspiral, merger, and ringdown parts. Usually, the inspiral waveform can be obtained by calibrating from post-Newtonian approximation; The merger and ringdown ones can be gotten from the quasinormal modes with black hole perturbation theory. However, for more general black holes, the calculation of the quasinormal modes is not trivial. In this paper we use the photon sphere to get the quasinormal modes of spinning black holes. Then we connect the ringdown wave with the inspiral part to get full waveforms and compare with the ones from numerical relativity. We find that they match with each other very well. In principle this method can be extended to some general compact objects. As an example, the ringdown waveforms from parametrized axisymmetric black holes are obtained. We also use this method to get the ringdown signals of the accelerating final black hole; this is due to gravitational recoil during the merger. Even for the extreme cases, the acceleration due to the recoil cannot produce detectable effects.
