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Comparison of cloud models for Brown Dwarfs

Published online by Cambridge University Press:  01 October 2007

Ch. Helling ,
A. Ackerman ,
F. Allard ,
M. Dehn ,
P. Hauschildt ,
D. Homeier ,
K. Lodders ,
M. Marley ,
F. Rietmeijer  and
T. Tsuji
...Show all authors
Ch. Helling
Affiliation:
SUPA, School of Physics & Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 9SS, Scotland, UK email: Christiane.Helling@st-andrews.ac.uk
A. Ackerman
Affiliation:
NASA Goddard Institute of Space Studies, New York, USA
F. Allard
Affiliation:
Centre de Recherche Astrophysique de Lyon, Université de Lyon, France
M. Dehn
Affiliation:
Hamburger Sternwarte, Hamburg, Germany
P. Hauschildt
Affiliation:
Hamburger Sternwarte, Hamburg, Germany
D. Homeier
Affiliation:
Universität Göttingen, Institut für Astrophysik, Göttingen, Germany
K. Lodders
Affiliation:
Planetary Chemsitry Laboratory, Department of Earth and Planetary Sciences, Washington University, St. Louis, USA
M. Marley
Affiliation:
NASA Ames Research Center, Moffett Field, USA
F. Rietmeijer
Affiliation:
Department of Earth and Planetary Sciences, University New Mexico, Albuquerque, USA
T. Tsuji
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo, Japan
P. Woitke
Affiliation:
UK Astronomy Technology Centre, Royal Observatory, Edinburgh, UK
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Abstract

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A test case comparison is presented for different dust cloud model approaches applied in brown dwarfs and giant gas planets. We aim to achieve more transparency in evaluating the uncertainty inherent to theoretical modelling. We show in how far model results for characteristic dust quantities vary due to different assumptions. We also demonstrate differences in the spectral energy distributions resulting from our individual cloud modelling in 1D substellar atmosphere simulations.

Keywords

astrochemistrymethods: numericalstars: atmospheresstars: low-massbrown dwarfs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 173 - 177
Copyright
Copyright © International Astronomical Union 2008

References

Ackerman, A. & Marly, M. 2001, ApJ 556, 872CrossRefGoogle Scholar
Allard, F., Allard, N. F., Homeier, D. et al. 2007, A&A 474, L21Google Scholar
Allard, F., Guillot, T., Ludwig, H.-G., Hauschildt, P. H., et al. 2003, IAU 211, 325Google Scholar
Dehn, M. 2007, PhD Thesis, University HamburgGoogle Scholar
Helling, Ch., Woitke, P., Thi, W.-F. 2008, submittedGoogle Scholar
Helling, Ch., Woitke, P. 2006, A&A 455, 325Google Scholar
Ludwig, H.-G., Allard, F., Hauschildt, P.H. 2002, A&A 395, 99Google Scholar
Sudarsky, D., Burrows, A., Hubeny, I. 2003, ApJ 588, 1121Google Scholar
Tsuji, T. 2005, ApJ 621, 1033CrossRefGoogle Scholar
Woitke, P., Helling, Ch. 2004, A&A 414, 335Google Scholar
Woitke, P., Helling, Ch. 2003, A&A 388, 297Google Scholar