AI 中文总结
本研究基于LISA观测大质量黑洞双体并合及后续遗迹搜索，通过黑洞自旋测量和引力波搜索，预测了标量与矢量超轻玻色子的质量限制及探测概率，为超轻玻色子的探测提供了前景。
AI 中文摘要
超轻玻色子可在旋转黑洞周围触发超辐射不稳定性，提取角动量，部分情况下产生可观测的引力波信号。当相关的自旋衰减时标短于黑洞寿命以及吸积等过程导致的自旋增长时标时，该过程会对黑洞自旋施加上限。此外，玻色云的形成与后续耗散会产生准连续的引力波辐射。本研究探索利用空间基LISA天文台对大质量黑洞双体并合的观测来限制和探测超轻玻色子的前景，考虑两种互补方法：对并合双体的黑洞自旋进行测量，以及针对大质量黑洞双体并合遗迹的后续引力波搜索。基于重种子或轻种子，本研究采用三种大质量黑洞的种群模型，预测标量玻色子和矢量玻色子的排除概率与探测概率。研究发现，黑洞自旋测量可限制标量玻色子质量在[5×10^-18,10^-14] eV范围内，矢量玻色子质量在[6×10^-19,2×10^-14] eV范围内，具体范围取决于模型；相比之下，若仅考虑矢量玻色子，后续引力波搜索对矢量玻色子质量的敏感范围更窄，约为[3×10^-17,3×10^-15] eV，具体数值同样取决于模型。若存在质量在[10^-16,2×10^-15] eV范围内的矢量玻色子，后续搜索可探测到的事件概率范围从极小到接近1，具体取决于天体物理模型。
英文摘要
Ultralight bosons can trigger superradiant instabilities around rotating black holes, extracting angular momentum and leading in some cases to observable gravitational signatures. When the associated spin-down timescale is shorter than the black hole lifetimes and the spin-up timescales due to, e.g. accretion, this process imposes an upper limit on black hole spins. In addition, the formation and subsequent dissipation of boson clouds generates quasi-continuous gravitational wave emission. In this work, we explore the prospects for constraining and detecting ultralight bosons with observations of massive black hole binary mergers with the space-based LISA observatory. We consider two complementary approaches: measurements of black hole spins from merging binaries and follow-up gravitational wave searches targeting massive black hole binary merger remnants. We consider three population models for massive black holes, based on either heavy or light seeds, and forecast the exclusion and detection probabilities for both scalar and vector bosons. We find that black hole spin measurements can constrain scalar masses in the range $[5\times10^{-18},10^{-14}]$ eV and vector masses in the range $[6\times10^{-19},2\times10^{-14}]$ eV, with the exact range depending on the model. In contrast, restricting to vector bosons, follow-up gravitational wave searches are sensitive to a narrower vector boson mass range of $\sim[3\times10^{-17},3\times10^{-15}]$ eV, with the specific values again depending on the model. If a vector boson with a mass in the range $[10^{-16},2\times10^{-15}]$ eV existed, the probability of having an event that the follow-up searches would be sensitive to ranges from very small to near unity depending on the astrophysical model.
