Observations of the Cooling of the Interstellar Gas

Phillips, T. G.

doi:10.1007/978-94-009-3861-8_26

T. G. Phillips³

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 134))

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Abstract

Cooling of the gas of the dense interstellar clouds takes place primarily at submillimeter wavelengths. At about 1mm cooling is due to the many rotational lines of heavy moleules, but at shorter wavelengths light molecules (hydrides) become the dominant species, with some assistance from the fine structure transitions of atomic carbon. Photodissociation regions at the surfaces of molecular clouds are cooled by fine structure transitions of atoms and atomic ions. A presentation is given of some aspects of the observed emission due to heavy molecules, light molecules, atoms and ions.

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California Institute of Technology, 320-47, Pasadena, California, USA
T. G. Phillips

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T. G. Phillips
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NASA Ames Research Center, Moffett Field, California, USA
David J. Hollenbach
Department of Physics and Astronomy, The University of Wyoming, Laramie, Wyoming, USA
Harley A. Thronson Jr.

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Phillips, T.G. (1987). Observations of the Cooling of the Interstellar Gas. In: Hollenbach, D.J., Thronson, H.A. (eds) Interstellar Processes. Astrophysics and Space Science Library, vol 134. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3861-8_26

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DOI: https://doi.org/10.1007/978-94-009-3861-8_26
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-277-2485-4
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