Abstract
We present a dynamical-chemical model of massive star-forming regions, in which gas and dust grains are included. We consider the last 10 5 . yr of the accretion phase of a protostellar object embedded in a dense and massive cloud with a density and temperature gradient. We follow the gas and grain chemical evolution of two collapsing shells of this cloud, until the end of the protostar accretion phase, at which time the density no longer increases. At this point, the temperature rises, the molecular mantles of the grains evaporate, and we follow the time evolution of the resultant gas chemistry. The scenario is based on earlier models of Millar, Brown, Charnley, and Tielens
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