Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...322..412b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 322, Nov. 1, 1987, p. 412-449.
Astronomy and Astrophysics
Astrophysics
512
Fluorescence, Hydrogen Clouds, Interstellar Gas, Molecular Spectra, Stellar Models, Emission Spectra, Infrared Spectra, Line Spectra, Molecular Clouds, Planetary Nebulae, Reflection Nebulae
Scientific paper
The infrared emission spectrum of H2 excited by ultraviolet absorption, followed by fluorescence, was investigated using comprehensive models of interstellar clouds for computing the spectrum and to assess the effects on the intensity to various cloud properties, such as density, size, temperature, and the intensity of the UV radiation field. It is shown that the absolute H2 IR line intensities depend primarily on the density of the cloud and the strength of the incident UV radiation, and to a much lesser exent on the temperature of the gas, the total thickness of the cloud, and the optical properties of the grains. A variety of recent observational results are discussed with reference to theoretical models. It is shown that the rich H2 emission spectrum of the reflection nebula NGC 2023 can be reproduced by a model with density of about 10,000/cu cm, temperature of about 80 K, and UV flux approximately 300 times that of the Galactic background starlight.
Black John Harry
van Dishoeck Ewine F.
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