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On the CH(+) ion in diffuse interstellar clouds
Lambert, D. L.; Danks, A. C.
AA(Texas, University, Austin), AB(European Southern Observatory, La Silla, Chile)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 303, April 1, 1986, p. 401-415. Research supported by the Robert A. Welch Foundation. (ApJ Homepage)
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NASA/STI Keywords:
Gas Density, Hydrocarbons, Interstellar Matter, Line Spectra, Molecular Clouds, Molecular Ions, Abundance, Interstellar Chemistry, Milky Way Galaxy, Reaction Kinetics, Southern Sky, Spectrum Analysis
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A survey of 65 lines of sight in the southern Milky Way for the interstellar line of CH(+) at 4232 A yielded 30 detections. The CH(+) column density N(CH+) is shown to be well correlated with the rotationally excited H2 detected by surveys with the Copernicus satellite: log N(CH+)/N(H2)ex inversely proportional to 2500/T(ex), where T(ex) is the excitation temperature of H2 provided by the observed populations in rotational levels J of about 3-5. This correlation is strong evidence that CH(+) is formed in warm gas where the reaction C(+) + H2 yields CH(+) + H is effective. Shocks probably provide the necessary heating.

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