Abstract
Chemical evolution of molecular clouds seems to be governed by both chemistry and dynamics. We briefly describe the basics of the coupled chemical-dynamical evolution. Current problems involving the simplest species, such as C, CO, O2 , H2O, in quiescent clouds are then discussed. We emphasize the simplest molecules, because their chemistry is much less uncertain than the chemistry of the larger, more complex molecules. This allows the role of dynamics to be elucidated with a little bit more confidence. A particularly interesting issue in this area is the possibility that a molecule or a suite of molecules may serve as signpost of quiescent dynamical evolution. It is recognized that complex molecules may be more useful for this purpose, once their chemistry is at least fairly understood. Energetic dynamical phenomenon, such as shocks, produce dramatic chemical signatures, such as the dramatically enhanced CH+ abundance, due to the opening of otherwise forbidden chemical reaction paths. As a corollary, chemistry may have the potential to improve our understanding of the impulsive dynamical processes in a significant manner. Equally impressive are the footprints of star formation on the chemical evolution of the parent dense cloud. This has been discussed with respect to the star forming region in the Orion. It seems possible that chemistry might act as a tracer of embedded protostellar or stellar objects which manage to elude direct observations.
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Prasad, S.S., Tarafdar, S.P., Villere, K.R., Huntress, W.T. (1987). Chemical Evolution of Molecular Clouds. In: Hollenbach, D.J., Thronson, H.A. (eds) Interstellar Processes. Astrophysics and Space Science Library, vol 134. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3861-8_23
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