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Molecular Hydrogen emission from protoplanetary disks: effects of X-ray irradiation and dust evolution

Published online by Cambridge University Press:  01 August 2006

H. Nomura ,
Y. Aikawa ,
M. Tsujimoto ,
Y. Nakagawa  and
T. J. Millar
H. Nomura
Affiliation:
Department of Earth and Planetary Sciences, Kobe University, Nada, Kobe 657-8501, Japan
Y. Aikawa
Affiliation:
Department of Earth and Planetary Sciences, Kobe University, Nada, Kobe 657-8501, Japan
M. Tsujimoto
Affiliation:
Department of Physics, Rikkyo University, Nishi-Ikebukuro, Toshima, Tokyo 171-8501, Japan
Y. Nakagawa
Affiliation:
Department of Earth and Planetary Sciences, Kobe University, Nada, Kobe 657-8501, Japan
T. J. Millar
Affiliation:
School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, Northern Ireland, UK
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Abstract

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We have made a detailed model of the physical structure of protoplanetary disks, taking into account X-ray and ultraviolet (UV) irradiation from a central star, as well as dust size growth and settling towards the disk midplane. Also, we calculate the level populations and line emission of molecular hydrogen from the disks, which shows that the dust evolution changes the physical properties of the disk, and then the line ratios of the molecular hydrogen emission.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 456
Copyright
Copyright © International Astronomical Union 2007

References

Aikawa, Y. & Nomura, H. 2006, ApJ 642, 1152CrossRefGoogle Scholar
Nomura, H. & Millar, T.J. 2005, A&A 438, 923Google Scholar