Eccentricity-driven modulation of the accretion and ejection processes. Top: 5-orbit evolution of the planet radius r_p (gray lines) and accretion rate in the planet gap 〈Ṁ〉_gap (purple lines) during two epochs in the run ℳ₂₀₀ : when the planet orbit is quasi-circular (thick lines) and once the planet eccentricity is nearly maximum (thin lines). Bottom: space-time diagram of the accretion rate Ṁ (left) and the ejection ℰ₊ at arctan(9h) (right) during the 5-orbit evolution of the eccentric giant planet. The instantaneous radial position of the planet is shown with white circles. Some characteristic velocities indicate how planet-driven waves are propagating in the disk: the adiabatic sound speed c_s in green and the Alfvén speed v_A in blue. The gap location used to compute ${\langle \dot{M}\rangle }_{\text{gap}}^{\text{ecc}}$ in the top panel is indicated by a white dashed rectangle in the bottom left panel.