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Although it is fairly established that Gravitational Instability (GI) shouldoccur in the early phases of the evolution of a protoplanetary disk, the fateof the clumps resulting from disk fragmentation and their role in planetformation is still unclear. In the present study we investigatesemi-analytically their evolution following the contraction of a syntheticpopulation of clumps with varied initial structure and orbits coupled with thesurrounding disk and the central star. Our model is based on recently publishedstate-of-the-art 3D collapse simulations of clumps with varied thermodynamics.Various evolutionary mechanisms are taken into account, and their effect isexplored both individually and in combination with others: migration and tidaldisruption, mass accretion, gap opening and disk viscosity. It is found that,in general, at least 50% of the initial clumps survive tides, leaving behindpotential gas giant progenitors after ~10^5 yr of evolution in the disk. Therest might be either disrupted or produce super-Earths and other low massplanets provided that a solid core can be assembled on a sufficiently shorttimescale, a possibility that we do not address in this paper. Extrapolating tomillion year timescales, all our surviving protoplanets would lead to close-ingas giants. This outcome might in part reflect the limitations of the migrationmodel adopted, and is reminiscent of the analogous result found incore-accretion models in absence of fine-tuning of the migration rate. Yet itsuggests that a significant fraction of the clumps formed by gravitationalinstability could be the precursors of Hot Jupiters.

Early evolution of clumps formed via gravitational instability in protoplanetary disks; precursors of Hot Jupiters?