The effects of nonthermal vibrational, rotational, and fine-structure distributions on the evolution of oxygen-bearing species in shocked interstellar clouds are investigated. Using a one-fluid treatment of the shock structure, we carry out a calculation of the rotational and vibrational populations of molecular hydrogen in the cooling gas. The rates specific to the vibrational, rotational, and fine-structure temperatures of the reactants are explicitly included for the principal oxygen-hydrogen reactions. Shocks of velocity 10 km s-1 propagating in clouds of initial densities 10, 103 , and 105 cm-3 with zero and moderate magnetic field strengths are considered in detail.
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Graff et al. (1987) studied this question.
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