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Chemical changes during transport from cloud to disk

Published online by Cambridge University Press:  01 February 2008

Ruud Visser ,
Ewine F. van Dishoeck  and
Steven D. Doty
Ruud Visser
Affiliation:
Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, the Netherlands email: [email protected]
Ewine F. van Dishoeck
Affiliation:
Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, the Netherlands email: [email protected] Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany
Steven D. Doty
Affiliation:
Department of Physics and Astronomy, Denison University, Olin Hall, Granville, OH 43023, USA
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Abstract

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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.

Keywords

Planetary systems: protoplanetary diskscircumstellar matterstars: formationastrochemistry
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S251: Organic Matter in Space , February 2008 , pp. 111 - 116
Copyright
Copyright © International Astronomical Union 2008

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