Abstract
Models of shocks in diffuse interstellar clouds are considered in which (a) the photodissociation of H2 is neglected, and (b) this process is included. Remaining discrepancies between the results of independent computer model calculations (Pineau des Forêts et al. 1986, Draine 1986) in category (a) are shown to relate to the assumed products of the photodissociation of CH+. We find that the rate of formation of CH+ in shocked gas is not significantly enhanced by the rotational excitation energy of the H2 molecule in the reaction C+ (H2(J),H) CH+ but is increased if the reaction CH+ (H2, H)CH +2 proceeds at appreciably less than the Langevin rate at high effective temperatures.
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© 1988 Kluwer Academic Publishers
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Flower, D.R., Monteiro, T.S., des Forêts, G.P., Roueff, E. (1988). Chemistry in Shocked Interstellar Gas. In: Millar, T.J., Williams, D.A. (eds) Rate Coefficients in Astrochemistry. Astrophysics and Space Science Library, vol 146. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3007-0_17
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DOI: https://doi.org/10.1007/978-94-009-3007-0_17
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