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Modeling giant planets and brown dwarfs

Published online by Cambridge University Press:  10 November 2011

Andreas Becker ,
Nadine Nettelmann ,
Ulrike Kramm ,
Winfried Lorenzen ,
Martin French  and
Ronald Redmer
Andreas Becker
Affiliation:
Institute of Physics, University of Rostock, Universitätsplatz 3, 18051, Rostock, Germany email: andreas.becker@uni-rostock.de
Nadine Nettelmann
Affiliation:
Dept. of Astronomy & Astrophysics, University of California, CA 95064 Santa Cruz, USA
Ulrike Kramm
Affiliation:
Institute of Physics, University of Rostock, Universitätsplatz 3, 18051, Rostock, Germany email: andreas.becker@uni-rostock.de
Winfried Lorenzen
Affiliation:
Institute of Physics, University of Rostock, Universitätsplatz 3, 18051, Rostock, Germany email: andreas.becker@uni-rostock.de
Martin French
Affiliation:
Institute of Physics, University of Rostock, Universitätsplatz 3, 18051, Rostock, Germany email: andreas.becker@uni-rostock.de
Ronald Redmer
Affiliation:
Institute of Physics, University of Rostock, Universitätsplatz 3, 18051, Rostock, Germany email: andreas.becker@uni-rostock.de
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Abstract

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We present new results in modeling the interiors of Giant Planets (GP) and Brown Dwarfs (BD). In general models of the interior rely on equation of state data for planetary materials which have considerable uncertainties in the high-pressure domain. Our calculations are based on ab initio equation of state (EOS) data for hydrogen, helium, hydrogen-helium mixtures and water as the representative of all heavier elements or ices using finite-temperature density functional theory molecular dynamics (FT-DFT-MD) simulations. We compare results for the BD Gliese 229B calculated with Saumon-Chabrier-Van Horn EOS (SCVH95) and our EOS data.

Keywords

equation of stateplanetary systemsbrown dwarfs

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