Comparison of models with fragmentation and bouncing with variable planet masses. Top left: evolution of the planetary mass in the time-dependent model. The solid line shows the default model where the planet reaches 20 M_⊕ at 1 Myr. The dashed line shows the evolution in a model with rapid early growth in which the planet reaches 40 M_⊕ at 1 Myr. Bottom left: fraction of outer disk dust mass accreted through the gap after 1 Myr in the default planetary mass evolution model for different values of dust diffusivity δ_r with fragmentation limited growth. Bottom right: solid lines show the fraction of outer disk material accreted through the gap after 1 Myr for bouncing limited growth for different values of the δ_i parameters in the default planetary growth model. The dashed green line shows a model of bouncing limited growth with δ_i = 10⁻⁵ and rapid early growth of the planet (dashed line in top left panel). The vertical lines indicate 4 Myr until which the two reservoirs needed to be separated. Top right: snapshot of the dust distribution at 4 Myr for the model with bouncing limited growth and δ_i = 10⁻⁵ (dashed green line in bottom right panel). The inner disk is depleted in dust and only supplied with small amounts of outer disk material.