Fraction of stars f_merger that merge with the central star in a cluster with a total stellar mass of M_stars = 10⁴ M_⊙ and a virial radius of R_v = 0.14 pc after 1 Myr (left panel), 2 Myr (middle panel), and 10 Myr (right panel) for different combinations of the number of stars N and the stellar radius R_star calculated using our model presented in Eq. (8). We can see that when the collisions are maintained for short periods of time, that is, 1 Myr, a massive object with ∼f_mergerM_stars = 0.15 × 10⁴ M_⊙ = 1500 M_⊙ is formed in the cluster center only when N is small (given that t_delay becomes larger than the integration time for large N) or large R_star. If the time limit is long, that is, 10 Myr, most of the clusters will form stars with ∼0.3 M_stars = 3000 M_⊙.