Final parsec problem of black hole mergers and ultralight dark matter
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arXiv
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| Hauptverfasser: | , , , , |
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| Format: | Preprint |
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2023
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| author | Koo, Hyeonmo Bak, Dongsu Park, Inkyu Hong, Sungwook E. Lee, Jae-Weon |
| author_facet | Koo, Hyeonmo Bak, Dongsu Park, Inkyu Hong, Sungwook E. Lee, Jae-Weon |
| contents | When two galaxies merge, they often produce a supermassive black hole binary (SMBHB) at their center. Numerical simulations with stars and cold dark matter show that SMBHBs typically stall out at a distance of a few parsecs apart and take billions of years to coalesce. This is known as the final parsec problem. We suggest that ultralight dark matter (ULDM) halos around SMBHBs can generate dark matter waves due to dynamical friction. These waves can effectively carry away orbital energy from the black holes, rapidly driving them together. To test this hypothesis, we performed numerical simulations of black hole binaries inside ULDM halos.
Due to gravitational cooling and quasi-normal modes, the loss-cone problem can be avoided. The decay time scale gives lower bounds on masses of the ULDM particles and SMBHBs comparable to observational data. Our results imply that ULDM waves can lead to the rapid orbital decay of black hole binaries. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2311_03412 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Final parsec problem of black hole mergers and ultralight dark matter Koo, Hyeonmo Bak, Dongsu Park, Inkyu Hong, Sungwook E. Lee, Jae-Weon Astrophysics of Galaxies When two galaxies merge, they often produce a supermassive black hole binary (SMBHB) at their center. Numerical simulations with stars and cold dark matter show that SMBHBs typically stall out at a distance of a few parsecs apart and take billions of years to coalesce. This is known as the final parsec problem. We suggest that ultralight dark matter (ULDM) halos around SMBHBs can generate dark matter waves due to dynamical friction. These waves can effectively carry away orbital energy from the black holes, rapidly driving them together. To test this hypothesis, we performed numerical simulations of black hole binaries inside ULDM halos. Due to gravitational cooling and quasi-normal modes, the loss-cone problem can be avoided. The decay time scale gives lower bounds on masses of the ULDM particles and SMBHBs comparable to observational data. Our results imply that ULDM waves can lead to the rapid orbital decay of black hole binaries. |
| title | Final parsec problem of black hole mergers and ultralight dark matter |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2311.03412 |