Rotating black holes can produce superradiant clouds of ultralight bosons. When the black hole is part of a binary system, its cloud can undergo resonances and ionization. These processes leave a distinct signature on the gravitational waveform that depends on the cloud’s properties. To determine the state of the cloud by the time the system enters the band of future millihertz detectors, we study the chronological sequence of resonances encountered during the inspiral. For the first time, we consistently take into account the nonlinearities induced by the orbital backreaction, and we allow the orbit to have generic eccentricity and inclination. We find that the resonance phenomenology exhibits striking new features. Resonances can “start” or “break” above critical thresholds of the parameters, which we compute analytically, and induce dramatic changes in eccentricity and inclination. Applying these results to realistic systems, we find two possible outcomes. If the binary and the cloud are sufficiently close to counterrotating, then the cloud survives in its original state until the system enters in band; otherwise, the cloud is destroyed during a resonance at large separations, but leaves an imprint on the eccentricity and inclination. In both scenarios, we characterize the observational signatures, with particular focus on future gravitational wave detectors.

中文翻译：

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黑洞双星中引力原子的共振历史


旋转黑洞可以产生超轻玻色子的超辐射云。当黑洞是双星系统的一部分时，它的云可以经历共振和电离。这些过程在重力波形上留下了明显的特征，该特征取决于云的特性。为了确定系统进入未来毫赫兹探测器频带时云的状态，我们研究了吸气过程中遇到的共振的时间顺序。我们第一次一致地考虑了轨道反反应引起的非线性，并且我们允许轨道具有通用的偏心率和倾角。我们发现共振现象学表现出惊人的新特征。共振可以“开始”或“突破”超过我们分析计算的参数临界阈值，并引起偏心率和倾角的巨大变化。将这些结果应用到现实系统中，我们发现两种可能的结果。如果双星系统和星云足够接近反向旋转，那么星云将保持其原始状态，直到系统进入带内；否则，云会在大间距共振期间被破坏，但会在偏心率和倾角上留下印记。在这两种情况下，我们都描述了观测特征，特别关注未来的引力波探测器。