Other
Scientific paper
Sep 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992natur.359..305p&link_type=abstract
Nature (ISSN 0028-0836), vol. 359, no. 6393, p. 305-307.
Other
11
H Ii Regions, Star Formation, Stellar Evolution, Stellar Mass, Galactic Halos, Globular Clusters, Mass Distribution, Molecular Clouds, Protostars, Star Clusters
Scientific paper
A model of star formation is presented in which the protostar phase ends when the protostar embedded in a condensing core of molecular gas interacts with another protostar or star and is ejected from its core. Such interactions must be important if stars preferentially form in dense but ultimately unbound protoclusters. In a simple model in which protostars accrete at a constant rate, the final distribution of stellar masses asymptotically approaches a simple universal distribution which is very similar to the observed mass function of stars. The general form of the mass function in this model is determined by a competition between accretion and collision rates, which provides a qualitative explanation for the differences in star formation in different environments.
Podsiadlowski Philipp
Price Nigel M.
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