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30 June-2 July 2009, Course on Origin of Solar System HYDRODYNAMICAL MODELS OF GIANT PLANET FORMATION NEAR STARS ⢠A major result of the hydrodynamical studies is that the proto-giant planets may pulsate and develop pulsation-driven mass loss. Only if the pulsations are damped can gas accretion produce Jupiter-mass envelopes. Extra-solar planets with a minimum of 0.5 MJ up, probably require efficient gas accretion and should satisfy the convective outer envelope criterion (Wuchterl 1993). ⢠Wuchterl (1993) has shown that almost all nebula conditions, from a literature collection of nebula models, result in radiative outer envelopes at the critical mass. Nonlinear radiation hydrodynamical calculations with zero-entropy gradient convection show that Uranus/Neptune-type giant planets are produced under such circumstances. Jupiter-mass planets should then be the exception. Max-Planck Institute for Solar System Research, Katlenburg-Lindau
