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Fig. 6


Top panel: azimuthally averaged surface density profile after the relaxation process for four selected models. The dashed black line shows the initial power-law distribution and the three vertical dotted lines mark the positions of the planets. Clearly visible is the joint gap that the giant planets create. While for h = 0.05 (blue, green), a density depression at the Neptune’s location is visible, this is not the case for the thicker disk with h = 0.07 (orange, red). The effect of viscosity in smoothing out density waves in the inner disk is visible as the difference between the blue and green line in the inner disk region. Bottom panel: eccentricity of rings in the same state for these models. We find that a larger scale-height leads to a lower initial eccentricity of the gap edge (blue vs. orange, green vs. red), while higherviscosity leads to slightly lower values (blue vs. green, orange vs. red).

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