Langer 1976

Langer, W.D., 1976: The carbon monoxide abundance in interstellar clouds. Astrophys. J., 206, 699-712.

The steady-state abundance of carbon monoxide in interstellar clouds is calculated as a function of optical depth, density, and temperature. The molecular reactions which lead to CO can be initiated by the following ion-molecule reactions: H⁺ + O → O⁺ + H, C⁺ + H2 → CH2⁺ + hν, and H₃⁺ + C and O. As the ultraviolet radiation field is attenuated, C⁺ is transformed primarily into CO and C I. There are characteristic column densities for the transition to CO corresponding to the optical depths for attenuating this field at different wavelengths. For thick, low-temperature clouds the attenuation of the fields which ionize carbon, sulfur, and heavy metals is important for CO production initiated by H₃⁺. Complete conversion to CO does not necessarily occur, and considerable neutral carbon may be expected even in optically thick clouds. Comparison of integrated column densities of CO with extinction are in reasonable agreement with observations.

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Langer, W.D.: The carbon monoxide abundance in interstellar clouds, Astrophys. J., 206, 699-712, 1976.

Langer, W.D. (1976), The carbon monoxide abundance in interstellar clouds, Astrophys. J., 206, 699-712.

Langer, W.D., 1976: The carbon monoxide abundance in interstellar clouds. Astrophys. J., 206, 699-712.

Langer, W.D. 1976, Astrophys. J., 206, 699.

Langer WD. The carbon monoxide abundance in interstellar clouds, Astrophys J 1976;206:699-712.

W.D. Langer, Astrophys. J. 206, 699-712 (1976).