Top panel: local flow rate of the dust mass in M_⊕ yr⁻¹ as a function of radius for a disk with a Jupiter mass planet at 31 au. For the low α-values 1 × 10⁻⁴ (red line), 5 × 10⁻⁴ (blue) and 1 × 10⁻³ (green), we observe that the bump outside the planet location is large enough to hold the dust from drifting toward the star, while for larger α-values 5 × 10⁻³ (yellow), 10⁻² (purple), there is only a weak accumulation outside the planetary gap. Bottom panel: cumulative dust mass contained within a radius r, as function of radius. For α-values 1 × 10⁻⁴, 5 × 10⁻⁴, 1 × 10⁻³, roughly all the mass of the disk is inside the bump that is created from the planet. For larger α-values 5 × 10⁻³, 1 × 10⁻², the bump is minimal and not able to hold the dust from drifting.