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Deci-Hz gravitational waves from the self-interacting axion cloud around a rotating stellar mass black hole
Hidetoshi Omiya, Takuya Takahashi, Takahiro Tanaka, and Hirotaka Yoshino
Phys. Rev. D 110, 044002 – Published 1 August 2024
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Abstract
Gravitational waves from condensates of ultralight particles, such as axions, around rotating black holes are a promising probe to search for unknown physics. For this purpose, we need to characterize the signal to detect the gravitational waves, which requires tracking the evolution of the condensates, including various effects. The axion self-interaction causes the nonlinear coupling between the superradiant modes, resulting in complicated branching of evolution. Most studies so far have considered evolution under the nonrelativistic approximation or the two-mode approximation. In this paper, we numerically investigate the evolution of the axion condensate without these approximations, taking higher multipole modes into account. We also investigate the possible signature in gravitational waves from the condensate. We show that the higher multipole modes are excited, leading to the gravitational wave signal by the transition of the axion between different levels. The most prominent signal of gravitational waves arises from the transition between modes with their angular quantum numbers different by two. The gravitational wave signal is emitted in the deci-Hz band for stellar mass black holes, which might be observable with the proposed gravitational wave detectors.
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- Received 7 May 2024
- Accepted 2 July 2024
DOI:https://doi.org/10.1103/PhysRevD.110.044002
© 2024 American Physical Society
Physics Subject Headings (PhySH)
- Research Areas
Classical black holesGravitational wave sources
- Physical Systems
Axion-like particles
Gravitation, Cosmology & Astrophysics
Authors & Affiliations
Hidetoshi Omiya1,*, Takuya Takahashi2,†, Takahiro Tanaka1,3,‡, and Hirotaka Yoshino4,5,§
- 1Department of Physics, Kyoto University, Kyoto 606-8502, Japan
- 2Department of Physics, Rikkyo University, Toshima, Tokyo 171-8501, Japan
- 3Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
- 4Department of Physics, Osaka Metropolitan University, Osaka 558-8585, Japan
- 5Nambu Yoichiro Institute of Theoretical and Experimental Physics (NITEP), Osaka Metropolitan University, Osaka 558-8585, Japan
- *Contact author: omiya@tap.scphys.kyoto-u.ac.jp
- †Contact author: ttakahashi1@rikkyo.ac.jp
- ‡Contact author: t.tanaka@tap.scphys.kyoto-u.ac.jp
- §Contact author: hyoshino@omu.ac.jp
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Issue
Vol. 110, Iss. 4 — 15 August 2024
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Images
Figure 1
Left: the behavior of as the function of , where denotes the real part of the frequency . The red and the blue solid curve correspond to the and fundamental superradiant modes, respectively. The corresponding dotted curves are the ones with the nonrelativistic approximation Eq.(15). The spin of the central black hole is set to . Right: the similar plot for the imaginary part of the frequencies .
Figure 2
The real part of the radial mode function, as a function of . The red and blue solid curves, respectively, correspond to the and superradiant modes without any approximation, while the dashed curves are the counterparts in the nonrelativistic approximation. The spin of the black hole and the mass of the axion are set to and , respectively. The phase of the mode functions is chosen so that there is no imaginary part for large .
Figure 3
Dissipative processes induced by the self-interaction. Each line represents an energy level. The left panel corresponds to the dissipation of the axion due to the absorption by the black hole, and the right panel corresponds to the dissipation due to the radiation to infinity. The particles in the cloud and make a transition to the one in the cloud and the dissipative mode specified by the superscript and .
Figure 4
An example of the time evolution of the normalized axion cloud mass . For clarity, we recovered the normalization of the cloud mass. The red solid, blue dashed, black dotted, and green dash-dotted curves correspond to the , 2, 3, and 4 modes, respectively. The initial black hole mass and black hole spin are and , respectively. We take the axion mass such that and the axion decay constant to be .
Figure 7
The parameter region where the effective growth rate for the () and the () are positive in the -plane. The blue and orange region corresponds to and , respectively. In the most of the overlapping region, holds.
Figure 8
The time evolution of the black hole spin parameters as functions of time. Top: the red solid, blue dashed, black dotted, and green dash-dotted curves correspond to the decay constant , and , respectively. The axion mass is chosen to satisfy . Middle: the same figure as the top one but with . Bottom: the same figure as the top one but with .
Figure 9
Frequencies of gravitational waves emitted from the axion condensates as functions of the axion mass . The blue circle corresponds to the pair annihilation of the fundamental mode. The yellow square, green diamond, red triangle, purple reversed triangle, brown open circle, and light blue open square correspond to the level transition signal of , , , , , , respectively. Here, corresponds to the mode labeled by , , and . Although overtones do not appear in our calculation, we show them for reference. The mass and spin of the black hole are fixed at and .
Figure 10
Left: the energy flux of the gravitational waves from various processes. Each point corresponds to the same process in Fig.9. (Right) The amplitude of the gravitational waves from various processes. Again, each point corresponds to the same process in Fig.9. The black hole is placed at .
Figure 11
Normalized masses of the axion clouds in the quasistationary configuration. The red solid, blue dotted, black dashed, and green dot-dashed curves correspond to the mass of the , 2, 3 and 4 cloud when the condensate is in the quasistationary configuration. The spin of the black hole is fixed at (top) and 0.7(bottom), respectively.
Figure 12
An example of the time evolution of the gravitational wave amplitude from an axion condensate. The red solid, blue dashed, and black dotted curves correspond to the time dependence of the gravitational wave amplitudes for the pair annihilation signal from the cloud, the level transition signals from the cloud to the cloud, and from the cloud to the cloud, respectively. We fix the initial black hole mass and spin at and 0.99. The axion mass and decay constant are and . The gravitational wave amplitude is estimated from the calculation setting the black hole spin to .
Figure 13
Upper left: the dependence of the peak amplitude of the gravitational wave from the pair annihilation signal of the cloud on axion mass and decay constant . The parameters of the black hole are taken to be the ones similar to Cygnus X-1, , and . We set a cutoff at . The upper ticks correspond to the . Upper right: the dependence of the duration of the pair annihilation signal, estimated by the FWHM, on and . The parameters of the black hole are the same as the upper left panel. Lower left: The similar figure as the upper left figure but with the initial black hole parameters similar to the black hole of GW170817. Namely, , and . We take the cutoff to be . Lower right: the same figure as the upper right figure but with the same parameters as the lower left figure.
Figure 14
The same figures as Fig.13, but with the gravitational waves from the level transition between the and the clouds.
Figure 15
The same figures as Fig.13, but with the gravitational waves from the level transition between the and the clouds.
Figure 16
The same figures as Fig.13, but with the gravitational waves from the level transition between the and the clouds.
Figure 17
Left: the blue solid and orange dotted curves show the amplitude of the axion wave normalized by the decay consent from the processes and , respectively. We set the black hole mass to and the spin to . We put the black hole to be 1kpc away from us. Right: same as the left panel but with number density flux.