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Chemical Evolution of a Protoplanetary Disk

Published online by Cambridge University Press:  21 December 2011

Dmitry A. Semenov
Dmitry A. Semenov*
Affiliation:
Max Planck Institute for Astronomy, Königstuhl 17, D–69117 Heidelberg, Germany email: [email protected]
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Abstract

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In this paper we review recent progress in our understanding of the chemical evolution of protoplanetary disks. Current observational constraints and theoretical modeling on the chemical composition of gas and dust in these systems are presented. Strong variations of temperature, density, high-energy radiation intensities in these disks, both radially and vertically, result in a peculiar disk chemical structure, where a variety of processes are active. In hot, dilute and heavily irradiated atmosphere only the most photostable simple radicals and atoms and atomic ions exist, formed by gas-phase processes. Beneath the atmosphere a partly UV-shielded, warm molecular layer is located, where high-energy radiation drives rich ion-molecule and radical-radical chemistry, both in the gas phase and on dust surfaces. In a cold, dense, dark disk midplane many molecules are frozen out, forming thick icy mantles where surface chemistry is active and where complex polyatomic (organic) species are synthesized. Dynamical processes affect disk chemical composition by enriching it in abundances of complex species produced via slow surface processes, which will become detectable with ALMA.

Keywords

accretion disksastrochemistrydiffusionline: formationmolecular processesprotoplanetary diskssubmillimetertechniques: interferometricturbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S280: The Molecular Universe , June 2011 , pp. 114 - 126
Copyright
Copyright © International Astronomical Union 2011

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