Simulating the Galactic population of axion clouds around stellar-origin black holes: Gravitational wave signals in the 10-100 kHz band
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| Main Authors: | , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866915156455325696 |
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| author | Sprague, Jacob R. Larson, Shane L. Wang, Zhiyuan Klomp, Shelby Laeuger, Andrew Winstone, George Aggarwal, Nancy Geraci, Andrew A. Kalogera, Vicky |
| author_facet | Sprague, Jacob R. Larson, Shane L. Wang, Zhiyuan Klomp, Shelby Laeuger, Andrew Winstone, George Aggarwal, Nancy Geraci, Andrew A. Kalogera, Vicky |
| contents | Ultralight scalar fields can experience runaway `superradiant' amplification near spinning black holes, resulting in a macroscopic `axion cloud' which slowly dissipates via continuous monochromatic gravitational waves. For a particular range of boson masses, $\mathcal{O}(10^{-11}$ -- $10^{-10})$ eV, an axion cloud will radiate in the $10$ -- $100$ kHz band of the Levitated Sensor Detector (LSD). Using fiducial models of the mass, spin, and age distributions of stellar-origin black holes, we simulate the present-day Milky Way population of these hypothetical objects. As a first step towards assessing the LSD's sensitivity to the resultant ensemble of GW signals, we compute the corresponding signal-to-noise ratios which build up over a nominal integration time of $10^{7}$ s, assuming the projected sensitivity of the $1$-m LSD prototype currently under construction, as well as for future $10$-m and $100$-m concepts. For a $100$-m cryogenic instrument, hundreds of resolvable signals could be expected if the boson mass $μ$ is around $3\times10^{-11}$ eV, and this number diminishes with increasing $μ$ up to $\approx 5.5\times10^{-11}$ eV. The much larger population of unresolved sources will produce a confusion foreground which could be detectable by a $10$-m instrument if $μ\in (3-4.5)\times10^{-11}$ eV, or by a $100$-m instrument if $μ\in (3-6)\times10^{-11}$ eV. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2409_03714 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Simulating the Galactic population of axion clouds around stellar-origin black holes: Gravitational wave signals in the 10-100 kHz band Sprague, Jacob R. Larson, Shane L. Wang, Zhiyuan Klomp, Shelby Laeuger, Andrew Winstone, George Aggarwal, Nancy Geraci, Andrew A. Kalogera, Vicky High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology Ultralight scalar fields can experience runaway `superradiant' amplification near spinning black holes, resulting in a macroscopic `axion cloud' which slowly dissipates via continuous monochromatic gravitational waves. For a particular range of boson masses, $\mathcal{O}(10^{-11}$ -- $10^{-10})$ eV, an axion cloud will radiate in the $10$ -- $100$ kHz band of the Levitated Sensor Detector (LSD). Using fiducial models of the mass, spin, and age distributions of stellar-origin black holes, we simulate the present-day Milky Way population of these hypothetical objects. As a first step towards assessing the LSD's sensitivity to the resultant ensemble of GW signals, we compute the corresponding signal-to-noise ratios which build up over a nominal integration time of $10^{7}$ s, assuming the projected sensitivity of the $1$-m LSD prototype currently under construction, as well as for future $10$-m and $100$-m concepts. For a $100$-m cryogenic instrument, hundreds of resolvable signals could be expected if the boson mass $μ$ is around $3\times10^{-11}$ eV, and this number diminishes with increasing $μ$ up to $\approx 5.5\times10^{-11}$ eV. The much larger population of unresolved sources will produce a confusion foreground which could be detectable by a $10$-m instrument if $μ\in (3-4.5)\times10^{-11}$ eV, or by a $100$-m instrument if $μ\in (3-6)\times10^{-11}$ eV. |
| title | Simulating the Galactic population of axion clouds around stellar-origin black holes: Gravitational wave signals in the 10-100 kHz band |
| topic | High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2409.03714 |