Introduction and Summary
Interstellar dust is an important component of the interstellar medium. It dominates the heating and cooling of clouds through energetic photoelectrons and gas-grain collisions (see the chapter by Black in this volume). It is also the dominant source of opacity and determines, therefore, the spectrum of dust-enshrouded objects. Unquestionably, molecular hydrogen, the most abundant gas-phase species in molecular clouds, is formed on grain surfaces. Other gas-phase molecules might result from reactions on grain surfaces as well. Grains can also influence the gas-phase composition of molecular clouds indirectly, because they may lock up some of the elements. The metals (e.g., iron) are particularly important in this respect since they tend to carry the charge inside a dense cloud and, thus, regulate the ion-molecule chemistry (see the chapter by Prasad in this volume). Such depletions will, of course, also influence the cooling balance.
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Tielens, A.G.G.M., Allamandola, L.J. (1987). Composition, Structure, and Chemistry of Interstellar Dust. 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_16
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