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Molecular hydrogen emission from protoplanetary disks: UV and X-ray irradiated disk model with dust evolution

Published online by Cambridge University Press:  06 January 2010

T. Montmerle ,
D. Ehrenreich ,
A.-M. Lagrange ,
H. Nomura ,
Y. Aikawa ,
M. Tsujimoto ,
Y. Nakagawa  and
T. J. Millar
H. Nomura
Affiliation:
ARC, School of Maths. and Physics, Queen's University Belfast, Belfast BT7 1NN, UK
Y. Aikawa
Affiliation:
Dept. of Earth and Planetary Sciences, Kobe University, Nada, Kobe 657-8501, Japan
M. Tsujimoto
Affiliation:
Dept. of Astronomy and Astrophysics, Pennsylvania State University, PA 16802, USA
Y. Nakagawa
Affiliation:
Dept. of Earth and Planetary Sciences, Kobe University, Nada, Kobe 657-8501, Japan
T. J. Millar
Affiliation:
ARC, School of Maths. and Physics, Queen's University Belfast, Belfast BT7 1NN, UK
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Abstract

We have modelled a detailed physical structure of protoplanetary disks, taking into account X-ray and UV irradiation from a central star, as well as dust size growth and settling towards the disk midplane. In addition, we have calculated the level populations and line emission of molecular hydrogen in the disks. As a result, we reproduce the observed strong H2 line flux if the disks are influenced by strong UV and X-ray irradiation. Also, the dust evolution changes the physical properties of the disk, and thus the H2 line ratios.


Type
Research Article
Information
European Astronomical Society Publications Series , Volume 41: Physics and Astrophysics of Planetary Systems , 2010 , pp. 181 - 184
Copyright
© EAS, EDP Sciences, 2010

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References

Nomura, H., Aikawa, Y., Tsujimoto, M., Nakagawa, Y., & Millar, T.J., 2007, ApJ, 661, 334 CrossRef
Nomura, H., & Millar, T.J., 2005, A&A, 438, 923