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The Chemistry of Nearby Disks

Published online by Cambridge University Press:  27 January 2016

Karin I. Öberg
Karin I. Öberg*
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St, MS 16, Cambridge, MA 02138 email: koberg@cfa.harvard.edu
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Abstract

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The gas and dust rich disks around young stars are the formation sites of planets. Observations of molecular trace species have great potential as probes of the disk structures and volatile compositions that together regulate planet formation. The disk around young star TW Hya has become a template for disk molecular studies due to a combination of proximity, a simple face-on geometry and richness in volatiles. It is unclear, however, how typical the chemistry of the TW disk is. In this proceeding, we review lessons learnt from exploring the TW Hya disk chemistry, focusing on the CO snowline, and on deuterium fractionation chemistry. We compare these results with new ALMA observations toward more distant, younger disks. We find that while all disks have some chemical structures in common, there are also substantial differences between the disks, which may be due to different initial conditions, structural or chemical evolutionary stages, or a combination of all three.

Keywords

astrochemistryprotoplanetary disksISM: moleculesradio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S314: Young Stars & Planets Near the Sun , November 2015 , pp. 143 - 148
Copyright
Copyright © International Astronomical Union 2016 

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