Comparison between a hydrodynamical and our dust evolution simulation for different α-values and for a planet/star mass ratio q = 10⁻³ at 30 au. In the left column are the different gap profiles for different α-values and in the right column the corresponding evolution tracks. Even though the profile from Kanagawa et al. (2016) does not overlapping with that obtained from the hydrodynamical simulation, the tracks in the right column produce similar results.