Top panels: mass-accretion rate (solid dark blue line) as a function of the orbital phase, t/P, during the last two simulated orbits for models Q2a02 to Q2e08. The eccentricity increases from left to right. The green dashed line corresponds to the BHL accretion rate as computed with Eq. (3) and α_BHL = 0.75. The dotted light blue line corresponds to the distance between the stars (right-hand scale). Middle panels: mass-loss rate as a function of time (solid red line) for the same models, measured as the flux crossing a sphere of radius 3a. The dotted pink line corresponds to the distance between the stars. Bottom panels: corresponding angular-momentum loss expressed by the parameter η as a function of time (solid yellow line). The distance between the star is shown with the dotted brown line. The dashed grey line corresponds to the isotropic-wind value η_iso = (1 + q)⁻², and the black dashed dotted line corresponds to the expected angular-momentum loss as computed by applying the fitting formula for angular-momentum loss from Paper II to the average orbital velocity.