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Formation of star clusters: Models and simulations

Part of: IAU Issue 315 - From Interstellar Clouds...

Published online by Cambridge University Press:  12 September 2016

Philip C. Myers
Philip C. Myers*
Affiliation:
Harvard-Smithsonian Center for Astrophysics 60 Garden Street, Cambridge, MA 02138USA email: pmyers@cfa.harvard.edu
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Abstract

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Recent progress is reviewed in describing the physical processes of star cluster formation, from the viewpoint of theoretical models and numerical simulations. In many studies, supersonic turbulent flows structure the gas into a network of clumps, filaments, and cores. Self-gravity drives star formation, moderated by turbulence, magnetic fields, and stellar feedback. Recent models and simulations describe the core mass function, the protostar mass function, and the star-formation rate. Several simulations indicate similar protostar birthrates, a mass advantage for firstborn protostars, and accretion rates that are superthermal and nearly constant. Recently observed core-filament systems with sonic line widths and parsec lengths present challenges for turbulent models.

Keywords

Molecular cloudsstar formationstar clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S315: From Interstellar Clouds to Star-Forming Galaxies: Universal Processes? , August 2015 , pp. 130 - 137
Copyright
Copyright © International Astronomical Union 2016 

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