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Comparison of cloud models for Brown Dwarfs

Published online by Cambridge University Press:  01 October 2007

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

Contributed Papers
Copyright © International Astronomical Union 2008


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