Dynamics of binary black holes in low-mass young star clusters

Young star clusters are dynamically active stellar systems and are a common birthplace for massive stars. Low-mass star clusters (similar to 300-10(3) M-circle dot) are more numerous than massive systems and are characterized by a two-body relaxation time-scale of a few Myr: the most massive stars sink to the cluster core and dynamically interact with each other even before they give birth to compact objects. Mere, we explore the properties of black holes (Buis) and binary black holes (BBHs) formed in low-mass young star clusters, by means of a suite of 10(5) direct N-body simulations with a high original binary fraction (100 per cent for stars with mass >5 M-circle dot). Most BM are ejected in the first similar to 20 Myr by dynamical interactions. Dynamical exchanges are the main formation channel of BBHs, accounting for similar to 40-80 per cent of all the systems. Most BBH mergers in low-mass young star clusters involve primary Buis with mass <40 M-circle dot and low-mass ratios are extremely more common than in the field. Comparing our data with those of more massive star clusters (10(3) - 3 x 10(4) M-circle dot), we find a strong dependence of the percentage of exchanged BBHs on the mass of the host star cluster. In contrast, our results show just a mild correlation between the mass of the host star cluster and the efficiency of BBH mergers.

Automated summary

Black holes (Buis) and binary black holes (BBHs) formed in low-mass young star clusters are mainly generated through dynamical exchanges, with most BBH mergers involving primary Buis with lower mass. The percentage of exchanged BBHs shows a strong dependence on the mass of the host star cluster, while the efficiency of BBH mergers only exhibits a mild correlation with the mass of the host star cluster, as indicated by the research data.