Computer Science
Scientific paper
Dec 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..353m&link_type=abstract
Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam
Computer Science
4
Scientific paper
We investigate the dynamical nature of protostellar outflows and their role in the evolution of a forming star cluster. We find that magnetic fields collimate protostellar winds into a common angular force distribution at distances sufficiently far from their source. Thin shells of gas swept into motion by these winds show features typically observed in protostellar outflows, in a wide variety of ambient density distributions, independently of wind intensity variations. This model of protostellar outflows predicts the mass ejected per star formed, and thus the efficiency of stellar cluster formation. Beginning with the mass ejection and energy injection implied by this model, and using the virial theorem as an equation of motion, we develop an approximate theory for the dynamical evolution of a cluster-forming molecular clump. Assuming that ambipolar diffusion regulates the star formation rate, we simulate the star--formation history of molecular clumps. The results compare favorably with the observations of gas motions in star forming clumps by Williams and Myers, and suggest a scenario for the formation of the Orion Nebula Cluster.
Matzner Christopher D.
McKee Christopher F.
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