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The final orbital position of growing planets is determined by theirmigration speed, which is essentially set by the planetary mass. Small massplanets migrate in type I migration, while more massive planets migrate in typeII migration, which is thought to depend mostly on the viscous evolution rateof the disc. A planet is most vulnerable to inward migration before it reachestype II migration and can lose a significant fraction of its semi-major axis atthis stage. We investigated the influence of different disc viscosities, thedynamical torque and gas accretion from within the horseshoe region asmechanisms for slowing down planet migration. Our study confirms that planetsgrowing in low viscosity environments migrate less, due to the earlier gapopening and slower type II migration rate. We find that taking the gasaccretion from the horseshoe region into account allows an earlier gap openingand this results in less inward migration of growing planets. Furthermore, thiseffect increases the planetary mass compared to simulations that do not takethe effect of gas accretion from the horseshoe region. Moreover, combining theeffect of the dynamical torque with the effect of gas accretion from thehorseshoe region, significantly slows down inward migration. Taking theseeffects into account could allow the formation of cold Jupiters (a > 1 au)closer to the water ice line region compared to previous simulations that didnot take these effects into account. We thus conclude that gas accretion fromwithin the horseshoe region and the dynamical torque play crucial roles inshaping planetary systems.

Probing the impact of varied migration and gas accretion rates for the formation of giant planets in the pebble accretion scenario