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Water in Protoplanetary Disks

Published online by Cambridge University Press:  29 April 2014

H. Nomura ,
C. Walsh ,
D. Heinzeller  and
T. J. Millar
H. Nomura
Affiliation:
Dept. of Astronomy, Graduate School of Science, Kyoto University, Kyoto 606-8502, Japan email: nomura@kusastro.kyoto-u.ac.jp
C. Walsh
Affiliation:
Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, University Road, Belfast, BT7 1NN, UK
D. Heinzeller
Affiliation:
MetService Ltd., 30 Sallamanca Rd. Kelburn, Wellington 6012, New Zealand
T. J. Millar
Affiliation:
Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, University Road, Belfast, BT7 1NN, UK
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Abstract

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Infrared water line emission from protoplanetary disks, recently observed by the Spitzer and Herschel space telescopes, is thought to trace the surface layer of the inner to outer regions of the disks. We have modelled the water abundance profile and line emission, especially focusing on the effects of dust size growth and turbulent mixing. Comparison between model calculations and observations suggests a small grain model with turbulent mixing is preferred.

Keywords

line: formationmolecular processesplanetary systems: protoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 235 - 237
Copyright
Copyright © International Astronomical Union 2014 

References

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