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On the structure and kinematics of molecular clouds from large scale mapping of mm-lines

Published online by Cambridge University Press:  03 August 2017

J. Bally ,
W. D. Langer ,
R. W. Wilson ,
A. A. Stark  and
M. W. Pound
J. Bally
Affiliation:
AT&T Bell Laboratories, HOH-L245, Holmdel, NJ 07733
W. D. Langer
Affiliation:
AT&T Bell Laboratories, HOH-L245, Holmdel, NJ 07733
R. W. Wilson
Affiliation:
AT&T Bell Laboratories, HOH-L245, Holmdel, NJ 07733
A. A. Stark
Affiliation:
AT&T Bell Laboratories, HOH-L245, Holmdel, NJ 07733
M. W. Pound
Affiliation:
AT&T Bell Laboratories, HOH-L245, Holmdel, NJ 07733

Abstract

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Molecular gas in the interior of the Orion superbubble consists of sheets, filaments, and partial shells in which the active star forming dense cloud cores are embedded. The main body of the Orion A and B clouds and at least 14 smaller clouds in Orion region are cometary in appearance suggesting strong interaction with massive stars in the Orion OB association. While the small scale (< 1 pc) structure of the clouds may be determined primarily by internal magnetic fields, gravity, and the effects of outflows from young stellar objects, the large scale morphology and kinematics is affected by the energy injected by massive stars. Supernovae, stellar winds, and radiation have compressed, accelerated, ablated, and dispersed molecular gas over the last 107 years. Most GMC/OB star complexes in the Solar neighborhood exhibit morphological and kinematic properties similar to the Orion region. We argue that energy injection by massive stars plays a vital role in the evolution of the ISM and may be responsible for much of the observed large-scale structure and kinematics of molecular clouds.

Type
Large Scale Structure
Information
Symposium - International Astronomical Union , Volume 147: Fragmentation of Molecular Clouds and Star Formation , 1991 , pp. 11 - 20
Copyright
Copyright © Kluwer 1991 

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