  Binary black holes (BHs) can be formed dynamically in the centers of star
clusters. The high natal kicks for stellar-mass BHs used in previous works made
it hard to retain BHs in star clusters. Recent studies of massive star
evolution and supernovae (SN) propose kick velocities that are lower due to the
fallback of the SN ejecta. We study the impact of these updates by performing
$N$-body simulations following instantaneous gas expulsion. For comparison, we
simulate two additional model sets with the previous treatment of stars: one
with high kicks and another with artificial removal of the kicks. Our model
clusters initially consist of about one hundred thousand stars, formed with
centrally-peaked efficiency. We find that the updated treatment of stars, due
to the fallback-scaled lower natal kicks, allows clusters to retain SN remnants
after violent relaxation. The mass contribution of the retained remnants does
not exceed a few percent of the total bound cluster mass during the early
evolution. For this reason, the first giga year of evolution is not affected
significantly by this effect. Nevertheless, during the subsequent long-term
evolution, the retained BHs accelerate mass segregation, leading to the faster
dissolution of the clusters.
