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During star cluster formation, ongoing mass accretion is resisted by stellarfeedback in the form of protostellar outflows from the low-mass stars andphoto-ionization and radiation pressure feedback from the massive stars. Wemodel the evolution of cluster-forming regions during a phase in which bothaccretion and feedback are present, and use these models to investigate howstar cluster formation might terminate. Protostellar outflows are the strongestform of feedback in low-mass regions, but these cannot stop cluster formationif matter continues to flow in. In more massive clusters, radiation pressureand photo-ionization rapidly clear the cluster-forming gas when its columndensity is too small. We assess the rates of dynamical mass ejection and ofevaporation, while accounting for the important effect of dust opacity onphoto-ionization. Our models are consistent with the census of protostellaroutflows in NGC 1333 and Serpens South, and with the dust temperatures observedin regions of massive star formation. Comparing observations of massivecluster-forming regions against our model parameter space, and against ourexpectations for accretion-driven evolution, we infer that massive-starfeedback is a likely cause of gas disruption in regions with velocitydispersions less than a few kilometers per second, but that more massive andmore turbulent regions are too strongly bound for stellar feedback to bedisruptive.

Star cluster formation with stellar feedback and large-scale inflow