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In the present paper we combine an N-body code that simulates the dynamics ofyoung dense stellar systems with a massive star evolution handler that accountsin a realistic way for the effects of stellar wind mass loss. We discuss twotopics:  1. The formation and the evolution of very massive stars (with a mass >120Mo) is followed in detail. These very massive stars are formed in the clustercore as a consequence of the successive (physical) collison of 10-20 mostmassive stars of the cluster (the process is known as runaway merging). Thefurther evolution is governed by stellar wind mass loss during core hydrogenburning and during core helium burning (the WR phase of very massive stars).Our simulations reveal that as a consequence of runaway merging in clusterswith solar and supersolar values, massive black holes can be formed but with amaximum mass of 70 Mo. In small metallicity clusters however, it cannot beexcluded that the runaway merging process is responsible for pair instabilitysupernovae or for the formation of intermediate mass black holes with a mass ofseveral 100 Mo.  2. Massive runaways can be formed via the supernova explosion of one of thecomponents in a binary (the Blaauw scenario) or via dynamical interaction of asingle star and a binary or between two binaries in a star cluster. We explorethe possibility that the most massive runaways (e.g., zeta Pup, lambda Cep,BD+433654) are the product of the collision and merger of 2 or 3 massive stars.

Stellar dynamics in young clusters: the formation of massive runaways and very massive runaway mergers