In the context of the core instability model and of the oli-garchic growth of solid protoplanets, we present a set of full evolu-tionary calculations of in situ giant planet formation. The growth of the core and the planetesimal accretion rate were coupled in a self–consistent way to the envelope's evolution. Several simulations for the formation of a Jupiter–like object were performed taking into account various surface densities for the protoplanetary disc and different sizes for the accreted planetesimals.
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