The dashed line in a) shows the boundaries of the initial disc while the solid line indicates the trajectory of a grazing perturber (r_peri/r_disc = 1) of equal mass (M₂/M₁ = 1). Material that resides within the disc after the perturbation is marked as black squares, while material that is in the end either bound to the perturbing star, unbound, or accreted is shown as grey dots. We note that the simulations were performed in three dimensions as can be seen in b).