The abundance of CH(+) in translucent molecular clouds - Further tests of shock models

Details The abundance of CH(+) in translucent molecular clouds - Further tests of shock models The abundance of CH(+) in translucent molecular clouds - Further tests of shock models

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...269..477g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 269, no. 1-2, p. 477-495.

Astronomy and Astrophysics

Astrophysics

97

Absorption Spectra, Hydrocarbons, Interstellar Matter, Molecular Clouds, Shock Wave Propagation, Astronomical Models, Molecular Ions

Scientific paper

Observations of interstellar absorption lines of CH(+) in the (0, 0) and (1, 0) bands of the A 1Pi - X 1Sigma(+) system are presented for 17 stars with reddenings up to E(B-V) about 1.5 mag. Complementary data on interstellar CH in the (0, 0) bands of the A 2Delta - X 2Pi and B 2Sigma(-) - X 2Pi systems and C2 in the A 1Pi(u) - X 1Sigma(g)(+) red system have been obtained as well. The derived CH(+) column densities continue to increase with total column density, and values up to 10 exp 14/sq cm are reported for highly-reddened lines of sight. In most cases, the CH(+) and CH absorptions are dominated by a single strong component, with weaker features displaced by a few km/s. No significant velocity difference is found between CH(+) and neutral species such as CH and CN for this sample of randomly oriented lines of sight. In contrast with CN, the CH(+) abundance does not increase with the density in the cloud as derived from the observed C2 excitation. For the two clouds with the largest density, HD 62542 and HD 94413, no CH(+) absorption is found with CH(+)/CH less than 0.03 and 0.14, respectively. The CH(+) findings do not support a single-shock origin for the formation of the ion.

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