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The Mopra DQS survey of the G333 region

Published online by Cambridge University Press:  01 August 2006

M. R. Cunningham ,
I. Bains ,
N. Lo ,
T. Wong ,
M. G. Burton  and
P. A. Jones
M. R. Cunningham
Affiliation:
School of Physics, University of New South Wales, NSW 2052, Australia email: [email protected]
I. Bains
Affiliation:
School of Physics, University of New South Wales, NSW 2052, Australia email: [email protected]
N. Lo
Affiliation:
School of Physics, University of New South Wales, NSW 2052, Australia email: [email protected] Australia Telescope National Facility, PO Box 76, Epping NSW 1710, Australia
T. Wong
Affiliation:
School of Physics, University of New South Wales, NSW 2052, Australia email: [email protected] Australia Telescope National Facility, PO Box 76, Epping NSW 1710, Australia
M. G. Burton
Affiliation:
School of Physics, University of New South Wales, NSW 2052, Australia email: [email protected]
P. A. Jones
Affiliation:
School of Physics, University of New South Wales, NSW 2052, Australia email: [email protected]
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Any successful model of star formation must be able to explain the low star forming efficiency of molecular clouds in our Galaxy. If the collapse of gas is regulated only by gravity, then the star formation rate should be orders of magnitude larger than the 1 M per year within our galaxy. The standard model invokes magnetic fields to slow down the rate of collapse, but does not explain star formation in cluster mode, or the lack of observed variations in the chemistry of molecular clouds if they are long-lived entities.

Keywords

ISM: cloudsturbulenceISM: moleculesradio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 404
Copyright
Copyright © International Astronomical Union 2007

References

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