Key points are not available for this paper at this time.
Recent observations of giant molecular cloud (GMC) cores suggest that star formation in the Galaxy may occur predominantly in dense protoclusters rather than in isolated low-mass cores. We present a model for the origin of stellar masses, based on interactions between young stellar objects in such a dense protocluster environment. We propose that collisions between protostellar cores (low-mass cores with central accreting protostars), and the passage of previously exposed protostars through the gaseous envelopes of protostellar cores, can eject protostars from their cores and terminate the main accretion phase. Using a simple model for the star-forming process, we construct analytic and numerical stellar initial mass functions that depend on the environment in which star formation occurs. The general form of these mass functions has a Salpeter-like power law and a high-mass exponential cut-off which depends on the environment, and is flat at small masses. Using a self-consistent, self-regulated star formation model to determine the rate of protostar formation and collision rates, we investigate the dependence of the initial mass function on the star formation environment (GMC cores, protoglobular clusters, high-mass star-forming regions). A model for the formation of binary stars, based on dynamical interactions between young stellar objects, is also suggested. It predicts a large binary formation frequency, with a wide range of eccentricities and periods. Limitations and possible extensions to the simple model are discussed, and its sensitivity to the model input parameters is examined.
Price et al. (Sat,) studied this question.