The Dragon-II simulations -- I. Evolution of single and binary compact objects in star clusters with up to 1 million stars

Abstract

We present the first results of the \textsc{Dragon-II} simulations, a suite of 19 $N$-body simulations of star clusters with up to $10^6$ stars, with up to $33\%$ of them initially paired in binaries. In this work, we describe the main evolution of the clusters and their compact objects (COs). All \textsc{Dragon-II} clusters form in their centre a black hole (BH) subsystem with a density $10-100$ times larger than the stellar density, with the cluster core containing $50-80\%$ of the whole BH population. In all models, the BH average mass steeply decreases as a consequence of BH burning, reaching values $⟨m_{\mathrm{BH}}⟩<15$ M${}_{\odot }$ within $10-30$ relaxation times. Generally, our clusters retain only BHs lighter than $30$ M${}_{\odot }$ over $30$ relaxation times. Looser clusters retain a higher binary fraction, because in such environments binaries are less likely disrupted by dynamical encounters. We find that BH-main sequence star binaries have properties similar to recently observed systems. Double CO binaries (DCOBs) ejected from the cluster exhibit larger mass ratios and heavier primary masses than ejected binaries hosting a single CO (SCOBs). Ejected SCOBs have BH masses $m_{\mathrm{BH}}=3-20$ M${}_{\odot }$, definitely lower than those in DCOBs ($m_{\mathrm{BH}}=10-100$ M${}_{\odot }$).

22 pages, 21 figures, 4 tables. Comments welcome. Submitted to MNRAS