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Protostellar turbulence in cluster forming regions of molecular clouds

Published online by Cambridge University Press:  01 August 2006

Fumitaka Nakamura  and
Zhi-Yun Li
Fumitaka Nakamura
Affiliation:
Faculty of Education and Human Sciences, Niigata University, 8050 Ikarashi-2, Niigata 950-2181, Japan, email: [email protected]
Zhi-Yun Li
Affiliation:
Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904, USA, email: [email protected]
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Abstract

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We perform 3D MHD simulations of cluster formation in turbulent magnetized dense molecular clumps, taking into account the effect of protostellar outflows. Our simulation shows that initial interstellar turbulence decays quickly as several authors already pointed out. When stars form, protostellar outflows generate and maintain supersonic turbulence that have a power-law energy spectrum of Ek ~ k−2, which is somewhat steeper than those of driven MHD turbulence simulations. Protostellar outflows suppress global star formation, although they can sometimes trigger local star formation by dynamical compression of pre-existing cores. Magnetic field retards star formation by slowing down overall contraction. Interplay of protostellar outflows and magnetic field generates large-amplitude Alfven and MHD waves that transform outflow motions into turbulent motions efficiently. Cluster forming clumps tend to be in dynamical equilibrium mainly due to dynamical support by protostellar outflow-driven turbulence (hereafter, protostellar turbulence).

Keywords

ISM: magnetic fieldsISM: cloudsMHDstars: formationturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 306 - 310
Copyright
Copyright © International Astronomical Union 2007

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