Same as Fig. 1, but for different aspect ratios, increasing from left to right, with α = 10⁻³. We note on the top of each row the difference in kinematic viscosity caused by the change in the disk’s aspect ratio (v = αh²r²Ω_K). The differences in the planetary accretion rates originate from the structure of the accretion formula itself (see Eq. (2)). At a low aspect ratio (h = 0.03, left panel), the accretion starts immediately in the second Machida regime. On the other hand, for h = 0.07, the change of accretion regime occurs at a higher mass and therefore at a later time, leading to a very different planet mass evolution.