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Merging hierarchical triple black hole systems with intermediate-mass black holes in population III star clusters.

Authors :
(刘帅), Shuai Liu
(王龙), Long Wang
(胡一鸣), Yi-Ming Hu
Tanikawa, Ataru
Trani, Alessandro A
Source :
Monthly Notices of the Royal Astronomical Society. Sep2024, Vol. 533 Issue 2, p2262-2281. 20p.
Publication Year :
2024

Abstract

Theoretical predictions suggest that very massive stars have the potential to form through multiple collisions and eventually evolve into intermediate-mass black holes (IMBHs) within Population III star clusters embedded in mini dark matter haloes. In this study, we investigate the long-term evolution of Population III star clusters, including models with a primordial binary fraction of |$f_{\rm b}=0$| and 1, using the N -body simulation code petar. We comprehensively examine the phenomenon of hierarchical triple black holes in the clusters, specifically focusing on their merging inner binary black holes (BBHs), with post-Newtonian correction, by using the tsunami code. Our findings suggest a high likelihood of the inner BBHs containing IMBHs with masses on the order of |$\mathcal {O}(100)\,{\rm M}_{\odot }$|⁠ , and as a result, their merger rate could be up to |$0.1{\rm Gpc}^{-3}{\rm yr}^{-3}$|⁠. The orbital eccentricities of some merging inner BBHs oscillate over time periodically, known as the Kozai–Lidov oscillation, due to dynamical perturbations. Detectable merging inner BBHs for mHz GW detectors LISA/TianQin/Taiji concentrate within |$z\lt 3$|⁠. More distant sources would be detectable for CE/ET/LIGO/KAGRA/DECIGO, which are sensitive from |$\mathcal {O}(0.1)$| Hz to |$\mathcal {O}(100)$| Hz. Furthermore, compared with merging isolated BBHs, merging inner BBHs affected by dynamical perturbations from tertiary BHs tend to have higher eccentricities, with a significant fraction of sources with eccentricities closing to 1 at mHz bands. GW observations would help constrain the formation channels of merging BBHs, whether through isolated evolution or dynamical interaction, by examining eccentricities. [ABSTRACT FROM AUTHOR]

Details

Language :
English
ISSN :
00358711
Volume :
533
Issue :
2
Database :
Academic Search Index
Journal :
Monthly Notices of the Royal Astronomical Society
Publication Type :
Academic Journal
Accession number :
179513364
Full Text :
https://doi.org/10.1093/mnras/stae1946