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We present a new model of giant planet formation that extends thecore-accretion model of Pollack etal (1996) to include migration, discevolution and gap formation. We show that taking into account these effects canlead to a much more rapid formation of giant planets, making it compatible withthe typical disc lifetimes inferred from observations of young circumstellardiscs. This speed up is due to the fact that migration prevents the severedepletion of the feeding zone as observed in in situ calculations. Hence, thegrowing planet is never isolated and it can reach cross-over mass on a muchshorter timescale. To illustrate the range of planets that can form in ourmodel, we describe a set of simulations in which we have varied some of theinitial parameters and compare the final masses and semi-major axes with thoseinferred from observed extra-solar planets.Comment: Accepted in Astronomy & Astrophysic

Models of giant planet formation with migration and disc evolution