Azimuthal average of the logarithm of the gas surface density ∑ for the run ℳ₃₀₀ , temporally averaged during a phase of quasi-circular and outward migration (dashed line), and during a phase of stalled and eccentric migration (solid line). The two vertical gray dotted lines show the reconstructed radii where the main sources of high-frequency Γ_Li variability are expected to originate from. The purple areas indicate the location of the inner and outer first-order external Lindblad resonances, for the modes m = 5 to m = 10. For the quasi-circular case (dashed line), the wind has already affected the planet gap, with a wider outer gap compared to the inner gap. For the eccentric case (solid line), the gap is globally denser due to the increase of the planet eccentricity. The wind has strongly enhanced the inner gap compared to the outer gap that is even further away from the planet location. The negative density gradient at the planet location could boost a negative corotation torque.