期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 480, 期 4, 页码 5645-5656出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty2211
关键词
globular clusters: general; stars: black holes; gravitational waves
资金
- China Postdoctoral Science Foundation [2017M610694]
- National Science Center (NCN), Poland [UMO-2015/17/N/ST9/02573]
- NCN, Poland [UMO-2016/23/B/ST9/02732]
- Carl Tryggers Foundation [CTS 17: 113]
- Foundation for Polish Science (FNP) [TEAM/2016-3/19]
- Lilly Endowment, Inc.
- Indiana METACyt Initiative
- International Space Science Institute (ISSI), Bern, Switzerland [393]
- U.S. National Science Foundation
- Italian Istituto Nazionale della Fisica Nucleare (INFN)
- French Centre National de Recherche Scientifique (CNRS)
- Dutch Nikhef
The dense environment of globular clusters (GCs) can facilitate the formation of binary black holes (BBHs), some of which can merge with gravitational waves within the age of the Universe. We have performed a survey of Monte Carlo simulations following the dynamical evolution of GCs with different masses, sizes, and binary fractions and explored the impact of the host GC properties on the formation of BBH mergers. We find that the number of BBH mergers from GCs is determined by the GC's initial mass, size, and primordial binary fraction. We identify two groups of BBH mergers: a primordial group whose formation does not depend on cluster's dynamics, and a dynamical group whose formation is driven by the cluster's dynamical evolution. We show how the BBH origin affects the BBH mergers' main properties such as the chirp mass and merging time distributions. We provide analytic expressions for the dependence of the number of BBH mergers from individual GCs on the main cluster's structural properties and the time evolution of the merger rates of these BBH5. These expressions provide an essential ingredient for a general framework allowing to estimate the merger rate density. Using the relations found in our study, we find a local merger rate density of 0.18-1.8 Crpc(-3) yr(-1) for primordial BBH mergers and 0.6-18 Gpc(-3) yr(-1) for dynamical BBH mergers, depending on the GC mass and size distributions, initial binary fraction, and the number density of GCs in the Universe.
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