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Aims. In the context of the core instability model, we present calculationsof in situ giant planet formation. The oligarchic growth regime of solidprotoplanets is the model adopted for the growth of the core. Methods. The fulldifferential equations of giant planet formation were numerically solved withan adaptation of a Henyey-type code. The planetesimals accretion rate wascoupled in a self-consistent way to the envelope's evolution. Results. Weperformed several simulations for the formation of a Jupiter-like object byassuming various surface densities for the protoplanetary disc and twodifferent sizes for the accreted planetesimals. We find that the atmosphericgas drag gives rise to a major enhancement on the effective capture radius ofthe protoplanet, thus leading to an average timescale reduction of 30% -- 55%and ultimately to an increase by a factor of 2 of the final mass of solidsaccreted as compared to the situation in which drag effects are neglected. Withregard to the size of accreted planetesimals, we find that for a swarm ofplanetesimals having a radius of 10 km, the formation time is a factor 2 to 3shorter than that of planetesimals of 100 km, the factor depending on thesurface density of the nebula. Moreover, planetesimal size does not seem tohave a significant impact on the final mass of the core.

Oligarchic planetesimal accretion and giant planet formation