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<p>Light bosons can form a gravitational atom (GA) around a spinning black hole through the superradiance proce ss. Considering the black hole to be part of a binary system, the tidal potential of the companion periodically perturbs the GA such that an “atomic” transition occurs between two of its energy eigenstates. The resonant transition is modeled by the Landau-Zener system, where the orbital frequency of the companion determines the relevant transition. In this work, we study a novel quasi-monochromatic gravitational wave signal originating directly from the level transition of the GA in a binary system. We derive the analytical formulae of both the strain waveform and frequency spectrum of the signal. We further investigate the GA-binary systems that can have a large signal-to-noise ratio in the milli-Hz to deci-Hz frequency band. Using the future space-based gravitational wave observatory DECIGO, we find the signal-to-noise ratio is 𝒪(10 – 200) for the fine-structure constant <i>α</i> ≃ 0<i>.</i>3, host black hole mass <i>M</i> = 150<i>M</i><sub>⊙</sub> and boson mass <i>μ</i> ≃ 10<sup>−13</sup>eV at a distance within 100 kpc. Given astrophysical uncertainties about the black hole’s initial spin, the degeneracy with other monochromatic signals and the small merger rate at those distances, we conclude that the detection of the signal would be challenging.</p>

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Gravitational waves from resonant transitions of tidally perturbed gravitational atoms

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  • 发表日期：

    2025年11月12日

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  • Antonios Kyriazis,
  • Fengwei Yang

摘要

Light bosons can form a gravitational atom (GA) around a spinning black hole through the superradiance proce ss. Considering the black hole to be part of a binary system, the tidal potential of the companion periodically perturbs the GA such that an “atomic” transition occurs between two of its energy eigenstates. The resonant transition is modeled by the Landau-Zener system, where the orbital frequency of the companion determines the relevant transition. In this work, we study a novel quasi-monochromatic gravitational wave signal originating directly from the level transition of the GA in a binary system. We derive the analytical formulae of both the strain waveform and frequency spectrum of the signal. We further investigate the GA-binary systems that can have a large signal-to-noise ratio in the milli-Hz to deci-Hz frequency band. Using the future space-based gravitational wave observatory DECIGO, we find the signal-to-noise ratio is 𝒪(10 – 200) for the fine-structure constant α ≃ 0.3, host black hole mass M = 150M⊙ and boson mass μ ≃ 10−13eV at a distance within 100 kpc. Given astrophysical uncertainties about the black hole’s initial spin, the degeneracy with other monochromatic signals and the small merger rate at those distances, we conclude that the detection of the signal would be challenging.