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Theory of Feedback in Clusters and Molecular Cloud Turbulence

Published online by Cambridge University Press:  27 April 2011

Enrique Vázquez-Semadeni
Enrique Vázquez-Semadeni*
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAM, Campus MoreliaP.O. Box 3-72 (Xangari), Morelia, Michoacán, México email: [email protected]
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Abstract

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I review recent numerical and analytical work on the feedback from both low- and high-mass cluster stars into their gaseous environment. The main conclusions are that i) outflow driving appears capable of maintaing the turbulence in parsec-sized clumps and retarding their collapse from the free-fall rate, although there exist regions within molecular clouds, and even some examples of whole clouds, which are not actively forming stars, yet are just as turbulent, so that a more universal turbulence-driving mechanism is needed; ii) outflow-driven turbulence exhibits specific spectral features that can be tested observationally; iii) feedback plays an important role in reducing the SFR; iv) nevertheless, numerical simulations suggest feedback cannot completely prevent a net contracting motion of clouds and clumps. Therefore, an appealing source for driving the turbulence everywhere in GMCs is the accretion from the environment, at all scales. In this case, feedback's most important role may be to prevent a fraction of the gas nearest to newly formed stars from actually reaching them, thus reducing the SFE.

Keywords

ISM: cloudsmethods: numericalstars: windsoutflowsturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 275 - 282
Copyright
Copyright © International Astronomical Union 2011

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