The formation of stellar clusters: Time-varying protostellar accretion rates

Identifying the processes that determine strength, duration, and variability of protostellar mass growth is a fundamental ingredient of any theory of star formation. I discuss protostellar mass accretion rates (M) over dot from numerical models that follow molecular cloud evolution from turbulent fragmentation toward the formation of stellar clusters. In a dense cluster environment, (M) over dot is strongly time varying and influenced by the mutual interaction of protostellar cores and their competition for accretion from the common cluster gas reservoir. Even for protostars with similar final mass, the accretion histories may differ dramatically. High-mass stars build up in the central parts of dense, cluster-forming cloud regions. They begin to form in the early phases of cluster evolution and continue to grow at a high rate until the available gas is exhausted or expelled by feedback. Lower mass stars tend to form at later phases, and (M) over dot declines rapidly after a short initial phase of strong growth. I present a simple fit formula for the time evolution of the average (M) over dot for protostars of different masses in a dense cluster environment.