Teen TITANS simulations -- I. Inefficient intermediate-mass black hole seeding via stellar collisions in young massive clusters

Abstract

Young massive clusters (YMCs) provide favorable environments for frequent stellar collisions, potentially leading to the formation of very massive stars (VMSs) and seeds of intermediate-mass black holes (IMBHs). We investigate the role of repeated stellar collisions in YMCs using TITANS, a new suite of 18 direct $N$-body simulations. Our models span cluster masses $10^5-10^6{\mathrm{M}}_{\odot }$, half-mass densities ${\rho }_{\mathrm{h}}=100-10^5{\mathrm{M}}_{\odot }\mathrm{p}{\mathrm{c}}^{-3}$, and include high primordial binary fractions, consistent with observations of massive stars in young clusters. Overall, our simulations assume cluster properties that are typical of YMCs in the low-redshift Universe. We find that repeated stellar collisions are efficient only in the densest clusters with short relaxation times and are absent in systems with ${\rho }_{\mathrm{h}}<500{\mathrm{M}}_{\odot }\mathrm{p}{\mathrm{c}}^{-3}$ and $t_{\mathrm{rh}}>1.3\mathrm{Gyr}$. Rapid mass segregation allows massive stars to sink to the cluster center, merge, and undergo subsequent collisions, even in clusters with long core-collapse times. However, collision chains are typically triggered by primordial binary mergers and usually involve only two collisions. In our simulations, only three VMSs form through repeated collisions and reach $m_{\ast }>330{\mathrm{M}}_{\odot }$, while most VMSs have $m_{\ast }<300{\mathrm{M}}_{\odot }$ and form through primordial binary mergers. None constitute viable IMBH seeds, as their helium cores fall in the (pulsational) pair-instability regime. We form five IMBHs from stellar collisions involving stars at different evolutionary stages, while the dominant channel is the merger of stellar-mass black holes, producing twelve IMBHs. For properties typical of local YMCs, stellar collision chains are therefore inefficient in producing IMBHs more massive than $140{\mathrm{M}}_{\odot }$, as most collisionally formed VMSs attain masses that fall in the pair-instability regime.

14 pages, 12 figures, 2 tables. Comments welcome