We present the first semi-analytical model that follows the chemical evolution during the collapse of a molecular cloud and the formation of a low-mass star and the surrounding disk. It computes infall trajectories from any starting point in the cloud and it includes a full time-dependent treatment of the temperature structure. We focus here on the freeze-out and desorption of CO and H2O. Both species deplete towards the centre before the collapse begins. CO evaporates during the infall phase and re-adsorbs when it enters the disk. H2O remains in the solid phase everywhere, except within a few AU of the star. Material that ends up in the planet- and comet-forming zones is predicted to spend enough time in a warm zone during the collapse to form complex organic species. © 2008 International Astronomical Union.
CITATION STYLE
Visser, R., Van Dishoeck, E. F., & Doty, S. D. (2008). Chemical changes during transport from cloud to disk. In Proceedings of the International Astronomical Union (Vol. 4, pp. 111–116). Cambridge University Press. https://doi.org/10.1017/S1743921308021297
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