Eccentric black hole mergers via three-body interactions in young, globular, and nuclear star clusters
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| Auteurs principaux: | , , , |
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| Format: | Preprint |
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2023
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| _version_ | 1866911801243860992 |
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| author | Dall'Amico, Marco Mapelli, Michela Torniamenti, Stefano Sedda, Manuel Arca |
| author_facet | Dall'Amico, Marco Mapelli, Michela Torniamenti, Stefano Sedda, Manuel Arca |
| contents | Eccentric mergers are a signature of the dynamical formation channel of binary black holes (BBHs) in dense stellar environments and hierarchical triple systems. Here, we investigate the formation of eccentric mergers via binary-single interactions by means of $2.5\times10^{5}$ direct $\textit{N}$-body simulations. Our simulations include post-Newtonian terms up to the 2.5th order and model the typical environment of young (YSCs), globular (GCs), and nuclear star clusters (NSCs). Around $0.6\%$ ($1\%$) of our mergers in NSCs (GCs) have an eccentricity ${>0.1}$ when the emitted gravitational wave frequency is 10 Hz in the source frame, while in YSCs this fraction rises to $1.6\%$. Approximately $\sim63\%$ of these mergers are produced by chaotic, resonant interactions where temporary binaries are continuously formed and destroyed, while $\sim31\%$ arise from an almost direct collision of two black holes (BHs). Lastly, $\sim 6\%$ of these eccentric mergers occur in temporary hierarchical triples. We find that binaries undergoing a flyby generally develop smaller tilt angles with respect to exchanges. This result challenges the idea that perfectly isotropic spin orientations are produced by dynamics. The environment dramatically affects BH retention: $0\%$, $3.1\%$, and $19.9\%$ of all the remnant BHs remain in YSCs, GCs, and NSCs, respectively. The fraction of massive BHs also depends on the host cluster properties, with pair-instability ($60\leq\,$M$_{\rm BH}$/M$_{\odot}\leq$100) and intermediate-mass (M$_{\rm BH}\geq$100$\,$M$_{\odot}$) BHs accounting for approximately $\sim44\%$ and $1.6\%$ of the mergers in YSCs, $\sim33\%$ and $0.7\%$ in GCs, and $\sim28\%$ and $0.4\%$ in NSCs, respectively. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2303_07421 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Eccentric black hole mergers via three-body interactions in young, globular, and nuclear star clusters Dall'Amico, Marco Mapelli, Michela Torniamenti, Stefano Sedda, Manuel Arca High Energy Astrophysical Phenomena Solar and Stellar Astrophysics General Relativity and Quantum Cosmology Eccentric mergers are a signature of the dynamical formation channel of binary black holes (BBHs) in dense stellar environments and hierarchical triple systems. Here, we investigate the formation of eccentric mergers via binary-single interactions by means of $2.5\times10^{5}$ direct $\textit{N}$-body simulations. Our simulations include post-Newtonian terms up to the 2.5th order and model the typical environment of young (YSCs), globular (GCs), and nuclear star clusters (NSCs). Around $0.6\%$ ($1\%$) of our mergers in NSCs (GCs) have an eccentricity ${>0.1}$ when the emitted gravitational wave frequency is 10 Hz in the source frame, while in YSCs this fraction rises to $1.6\%$. Approximately $\sim63\%$ of these mergers are produced by chaotic, resonant interactions where temporary binaries are continuously formed and destroyed, while $\sim31\%$ arise from an almost direct collision of two black holes (BHs). Lastly, $\sim 6\%$ of these eccentric mergers occur in temporary hierarchical triples. We find that binaries undergoing a flyby generally develop smaller tilt angles with respect to exchanges. This result challenges the idea that perfectly isotropic spin orientations are produced by dynamics. The environment dramatically affects BH retention: $0\%$, $3.1\%$, and $19.9\%$ of all the remnant BHs remain in YSCs, GCs, and NSCs, respectively. The fraction of massive BHs also depends on the host cluster properties, with pair-instability ($60\leq\,$M$_{\rm BH}$/M$_{\odot}\leq$100) and intermediate-mass (M$_{\rm BH}\geq$100$\,$M$_{\odot}$) BHs accounting for approximately $\sim44\%$ and $1.6\%$ of the mergers in YSCs, $\sim33\%$ and $0.7\%$ in GCs, and $\sim28\%$ and $0.4\%$ in NSCs, respectively. |
| title | Eccentric black hole mergers via three-body interactions in young, globular, and nuclear star clusters |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2303.07421 |