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arXiv · astro-ph/0603278

Equilibrium Star Cluster Formation

Jonathan C. Tan·Mark R. Krumholz·Christopher F. McKee
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Abstract

We argue that rich star clusters take at least several local dynamical times to form, and so are quasi-equilibrium structures during their assembly. Observations supporting this conclusion include morphologies of star-forming clumps, momentum flux of protostellar outflows from forming clusters, age spreads of stars in the Orion Nebula Cluster (ONC) and other clusters, and the age of a dynamical ejection event from the ONC. We show that these long formation timescales are consistent with the expected star formation rate in turbulent gas, as recently evaluated by Krumholz & McKee. Finally, we discuss the implications of these timescales for star formation efficiencies, the disruption of gas by stellar feedback, mass segregation of stars, and the longevity of turbulence in molecular clumps.

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Jonathan C. Tan, Mark R. Krumholz, Christopher F. McKee. 2006-03-10. Equilibrium Star Cluster Formation. https://doi.org/10.1086/504150

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