Velocity distribution of companions ejected after their MS. Helium stars and white dwarfs (WD) can have much shorter pre-CC orbits because of their smaller radii, and thus they can reach much higher ejection velocities. Conversely, the number of non-degenerate, hydrogen-rich post-MS stars is dominated by red supergiants with very large radii, which can only exist at large separation from the exploding companion, and thus typically have much slower velocities. Top panel: corresponding cumulative distributions.