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

Abstract

Young star clusters are dynamically active stellar systems and are a common birthplace for massive stars. Low-mass star clusters ($\sim 300-10^3$ M${}_{\odot }$) 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. Here, we explore the properties of black holes (BHs) 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 % for stars with mass $>5$ M${}_{\odot }$). Most BHs are ejected in the first $\sim 20$ Myr by dynamical interactions. Dynamical exchanges are the main formation channel of BBHs, accounting for $\sim 40-80$ % of all the systems. Most BBH mergers in low-mass young star clusters involve primary BHs with mass $<40$ M${}_{\odot }$ and low mass ratios are extremely more common than in the field. Comparing our data with those of more massive star clusters ($10^3-3\times 10^4$ M${}_{\odot }$), 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.

arXiv comment14 pages, 13 figures, comments welcome

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