Abstract
The chemical processes which accompany the birth of new stars from dense molecular clouds are discussed. Basic molecular processes are summarized and recent developments in gas-phase and gas-grain models are reviewed. In dark pre-stellar cores, long carbon-chain molecules produced by low temperature ion-molecule and neutral-neutral reactions are found to be abundant. During the cold collapse phase, most species are depleted onto the grains, where subsequent grain-surface reactions can produce hydrogenated molecules. The amount of depletion is difficult to determine observationally, but new constraints on the abundances and composition of the ices are obtained from the ISO data. Once the young star heats up its surroundings, the ices start to evaporate back into the gas phase, with the most volatile species returned first. These molecules drive a rapid hot core chemistry, resulting in complex organic species such as CH3OCH3. Shocks created by the interaction of the outflow with the envelope return both refractory and mantle material to the gas. The observational tools for probing each of the phases are discussed.
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Van Dishoeck, E.F. (1999). Models and Observations of Gas-Grain Interactions in Star-Forming Regions. In: Greenberg, J.M., Li, A. (eds) Formation and Evolution of Solids in Space. NATO ASI Series, vol 523. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4806-1_6
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