Axion clouds may survive the perturbative tidal interaction over the early inspiral phase of black hole binaries
Axion clouds may survive the perturbative tidal interaction over the early inspiral phase of black hole binaries
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DOI：
10.1088/1475-7516/2021/10/031
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发表时间：
2021-06
影响因子：
6.4
通讯作者：
Takuya Takahashi;Takahiro Tanaka
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文献类型：
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作者：
Takuya Takahashi;Takahiro Tanaka
引力波观测有可能探测超轻玻色场，如轴子。轴子通过超辐射不稳定性在旋转黑洞(BH)周围形成云，应该会影响来自双星BH的引力波形。另一方面，考虑双星系统中与BH相关联的云，潮汐相互作用在某些情况下会在激发相耗尽云。在假定只有主导的四极潮汐扰动作为第一步的情况下，我们对等质量双星在较宽的参数范围内的云损耗进行了详尽的数值研究。在这个假设下，我们发现只有当(1)指方位角动量本征值为+1的最低束缚态的L=1模是最快增长的模，(2)双轨道相对于BH自旋是逆旋转的，以及(3)云处于非相对论区域时，云才能避免由于潮汐效应而消失。
Gravitational wave observation has the potential of probing ultralight bosonic fields such as axions. Axions form a cloud around a rotating black hole (BH) by superradiant instability and should affect the gravitational waveform from binary BHs. On the other hand, considering the cloud associated with a BH in a binary system, tidal interaction depletes the cloud in some cases during the inspiral phase. We made an exhaustive study of the cloud depletion numerically in a wide parameter range for equal mass binaries, assuming only the leading quadrupolar tidal perturbation is at work as a first step. Under this assumption, we found that clouds can avoid disappearing due to the tidal effect only when (1) the l = 1 mode, which refers to the lowest bound state with the azimuthal angular momentum eigenvalue being +1, is the fastest growing mode, (2) the binary orbit is counter-rotating relative to the BH spin and (3) the cloud is in the non-relativistic regime.