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Chemistry in Protoplanetary Disks

Published online by Cambridge University Press:  30 March 2016

Yuri Aikawa*
Affiliation:
Department of Earth and Planetary Sciences, Kobe University, Kobe 657-8501, Japan

Abstract

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Molecular evolution is calculated in migrating fluid parcels in a protoplanetary disk considering gas-phase and grain-surface reactions. Radial distribution of molecules is obtained, which depends on ionization rate, temperature and/or desorption rate in the disk. If the temperature is high enough (> 20 K) or non-thermal desorption is efficient enough to sublimate dominant species such as CO in the comet forming regions, the desorbed species are transformed to less volatile species and again incorporated into ice mantles. Chemistry in these outer disks is similar to that in molecular clouds; it produces both oxidized and reduced species with a high D/H ratio.

Type
I. Joint Discussions
Copyright
Copyright © Astronomical Society of Pacific 2005

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