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Chemical evolution of molecular cloudsThe principles behind the coupled chemical-dynamical evolution of molecular clouds are described. Particular attention is given to current problems involving the simplest species (i.e., C. CO, O2, and H2) in quiescent clouds. The results of a comparison made between the molecular abundances in the Orion ridge and the hot core (Blake, 1986) are presented.
Document ID
19880027297
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Prasad, Sheo S.
(California Institute of Technology, Jet Propulsion Laboratory, Pasadena; Aerojet Electrosystems Co., Azusa CA, United States)
Tarafdar, Sankar P.
(Tata Institute of Fundamental Research Bombay, India)
Villere, Karen R.
(San Francisco State University CA, United States)
Huntress, Wesley T., Jr.
(California Institute of Technology Jet Propulsion Laboratory, Pasadena, United States)
Date Acquired
August 13, 2013
Publication Date
January 1, 1987
Subject Category
Astrophysics
Meeting Information
Meeting: Interstellar processes
Location: Grand Teton National Park, WY
Country: United States
Start Date: July 1, 1986
End Date: July 7, 1986
Accession Number
88A14524
Distribution Limits
Public
Copyright
Other

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