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Convection during the formation of gaseous giants and stars

Published online by Cambridge University Press:  01 August 2006

Günther Wuchterl
Günther Wuchterl*
Affiliation:
Thüringer Landessternwarte Tautenburg Sternwarte 5, D–07778 Tautenburg, Germany email: gwuchterl@TLS-Tautenburg.de
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Abstract

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Convection theories for star and planet formation studies have to be (1) simple, to allow a self-consistent solution with other relevant processes, (2) time-dependent, because convection often starts in collapse-flows, and (3) robust, i.e. physically well-behaved under a wide range of conditions ranging from the quiet protoplanetary nebula to supercritical protostellar accretion-shocks with Mach-numbers of a few hundred. I describe how the equations of radiation fluid-dynamics can be augmented by a one-equation convection model in order to construct a system of equations that contains the Sun, brown dwarfs and planets as well as their nearly isothermal parent-clouds. The system of equations is calibrated to the Sun and tested by the solar convection zone and the pulsations of RR-Lyrae stars. I discuss the following applications: (1) star formation as the collapse of Bonnor-Ebert spheres of masses ranging from the stellar domain to the brown dwarf region, (2) the approach to the main sequence, (3) companion mass determinations for direct imaging searches for exoplanets, with GQ Lupi as an example, and (4) the formation of Pegasi-planets, and the “large core” exoplanet, HD 149 026, in particular.

Keywords

Convectionplanets and satellites: formationsolar system: formationstars: formationstars: pre–main-sequence(stars:) planetary systems: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 211 - 216
Copyright
Copyright © International Astronomical Union 2007

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