Abstract
Much of the baryonic matter in the universe is in the form of H2, which includes most of the gas in Galactic and extragalactic interstellar clouds. Molecular hydrogen plays a significant role in establishing the thermal balance in many astrophysical environments and can be important as a spectral diagnostic of the gas. Modeling and interpretation of observations of such environments requires a quantitatively complete and accurate treatment of H2. Using this microphysical model of H2, we present illustrative calculations of prototypical astrophysical environments. This work forms the foundation for future investigations of these and other environments in which H2 is an important constituent.
Document Type
Article
Publication Date
5-10-2005
Digital Object Identifier (DOI)
http://dx.doi.org/10.1086/429215
Repository Citation
Shaw, G.; Ferland, Gary J.; Abel, N. P.; Stancil, P. C.; and van Hoof, P. A. M., "Molecular Hydrogen in Star-Forming Regions: Implementation of its Microphysics in CLOUDY" (2005). Physics and Astronomy Faculty Publications. 93.
https://uknowledge.uky.edu/physastron_facpub/93
Notes/Citation Information
Published in The Astrophysical Journal, v. 624, no. 2, p. 794-807.
© 2005. The American Astronomical Society. All rights reserved. Printed in the U.S.A.
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