Vibrationally excited molecular hydrogen in circumstellar clouds and the interstellar CH/+/ abundance

Details Vibrationally excited molecular hydrogen in circumstellar clouds and the interstellar CH/+/ abundance Vibrationally excited molecular hydrogen in circumstellar clouds and the interstellar CH/+/ abundance

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ap%26ss..83..417f&link_type=abstract

Astrophysics and Space Science, vol. 83, no. 1-2, Apr. 1982, p. 417-422.

Astronomy and Astrophysics

Astrophysics

10

Hydrogen Clouds, Interstellar Chemistry, Interstellar Gas, Molecular Ions, Stellar Envelopes, Ultraviolet Radiation, Abundance, Gas Density, Stellar Models

Scientific paper

The mechanism for forming interstellar CH(+) via the reaction proposed by Stecher and Williams (1972, 1974) is studied, particularly for the star 20 Tau and the cloud of molecular hydrogen closely associated with it. It is shown that the abundance of molecular hydrogen necessary to account for typical observed CH(+) column densities arising from the proposed reaction is not in conflict with observations of molecular hydrogen. The cloud required by the model must be in the form of a dense sheet with density 100,000/cu cm and thickness of about 0.02 pc. The dissipation time for such a sheet, in the absence of restraining mechanisms, is short. Thus, this model appears to require a rather special situation to satisfy the observations.

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