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G. Wuchterl (MPE - Max-Planck-Institut fuer extraterrestrische Physik)
Their expected luminosities make nearby young giant planets favorable for the first direct detection of an extrasolar planet. The giant planet formation process is relatively slow with expected formation times ranging from comparable to the star formation timescale up to the nebula lifetime, depending on the formation theory. Therefore quantitative models of giant planet formation and star formation are needed to determine the properties of young giant planets orbiting young stars for ages less than 100 Myr. I present new hydrodynamical calculations of the formation and early evolution of giant planets, giant gaseous protoplanets, brown dwarfs and stars. These models use the equations of radiation-fluid dynamics in spherical symmetry and include a new time-dependent description of convection that was successfully tested for the Sun and RR-Lyrae stars. Based on the results I discuss the nature of sample faint companion candidates in the TW Hydrae association.
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