Snapshots of the logarithmic density of an accretion disc surrounding the primary black hole of a pre-CBD BBH. The secondary black hole orbiting in a circular motion around the primary black hole (in the frame of the primary black hole) has an equal mass (q = 1), while being separated by D₁₂ = 2000 r_g1. Time here is normalised to the BBH period P_BBH. The tidal effects induced by the presence of the secondary object leads to the removal of the outer part of the initial disc whose outer edge lies beyond the Lagrangian L₁ point of the BBH. After more than one orbital period of the BBH, the disc remains stable with an outer edge reduced to approximately 600 r_g1, while displaying an elliptic outer edge shape whose eccentricity is e = 0.52 ± 0.12.