Scan of the surface imaginary part of the potential perturbation for a limited portion of the orbital rotation rate. The system studied is a twin binary system composed of 3.5 M_⊙ stars with a stellar rotation frequency of 0.25 Ω_crit = 5.95 d⁻¹ and an orbital eccentricity of e = 0.4. The top panel corresponds to positive values of the potential perturbation, while the lower panel corresponds to negative values. In the upper part of the figure, the identification of the dominant oscillation can be found and is noted g radial order (k). In this figure, the amplitudes of all the oscillation modes have been divided by k to magnify their width.