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Molecules in star formation

Published online by Cambridge University Press:  25 May 2016

F.H. Shu
F.H. Shu*
Affiliation:
Astronomy Department, University of California, Berkeley, CA 94720-3411, USA

Abstract

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We review current ideas and models in the problem of star formation from molecular cloud cores that are relatively isolated from the influences of other forming stars. We discuss the time scales, flow dynamics, and density and temperature structures applicable to each of the four stages of the entire process: (a) formation of a magnetized cloud core by ambipolar diffusion and evolution to a pivotal state of gravomagneto catastrophe; (b) self-similar collapse of the pivotal configuration and the formation of protostars, disks, and pseudo-disks; (c) onset of a magnetocentrifugally driven, lightly ionized wind from the interaction of an accretion disk and the magnetosphere of the central star, and the driving of bipolar molecular outflows; (d) evolution of pre-main-sequnce stars surrounded by dusty accretion disks. For each of these stages and processes, we consider the characteristics of the molecular diagnostics needed to investigate the crucial aspects of the observational problem.

Type
Star Formation
Information
Symposium - International Astronomical Union , Volume 178: Molecules in Astrophysics: Probes and Processes , 1997 , pp. 19 - 30
Copyright
Copyright © Kluwer 1997 

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