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The core accretion mechanism is presently the most widely accepted cause ofthe formation of giant planets. For simplicity, most models presently assumethat the growth of planetary embryos occurs in isolation. We explore how thesimultaneous growth of two embryos at the present locations of Jupiter andSaturn affects the outcome of planetary formation. We model planet formation onthe basis of the core accretion scenario and include several key physicalingredients. We consider a protoplanetary gas disk that exponentially decayswith time. For planetesimals, we allow for a distribution of sizes from 100~mto 100~km with most of the mass in the smaller objects. We include planetesimalmigration as well as different profiles for the surface density $\Sigma$ of thedisk. The core growth is computed in the framework of the oligarchic growthregime and includes the viscous enhancement of the planetesimal capturecross-section. Planet migration is ignored. By comparing calculations assumingformation of embryos in isolation to calculations with simultaneous embryogrowth, we find that the growth of one embryo generally significantly affectsthe other. This occurs in spite of the feeding zones of each planet neveroverlapping. The results may be classified as a function of the gas surfacedensity profile $\Sigma$: if $\Sigma \propto r^{-3/2}$ and the protoplanetarydisk is rather massive, Jupiter's formation inhibits the growth of Saturn. If$\Sigma \propto r^{-1}$ isolated and simultaneous formation lead to verysimilar outcomes; in the the case of $\Sigma \propto r^{-1/2}$ Saturn growsfaster and induces a density wave that later acclerates the formation ofJupiter. Our results indicate that the simultaneous growth of several embryosimpacts the final outcome and should be taken into account by planet formationmodels.

Consequences of the simultaneous formation of giant planets by the core accretion mechanism