We conclude to have found evidence of periodic line-profile variability in the primary and secondary of CV Vel with a period between 5.7 and 6.4 days. This is almost equal to the orbital period. Moreover, the quoted frequency error is a formal 1σ leastsquares error, and is an underestimation of the true error given that we covered less than two full cycles with unblended Mg II lines. It therefore seems that line-profile variability occurs with a period very close or equal to the orbital one. This is potentially interesting as it could point towards the excitation of a tidally induced g-mode oscillation in the components. However, given the phase relation we obtained, and the absence of any periodic signature in < v 2 >, it is more likely that a reflection and/or variable limb-darkening effect lies at the origin of the detected variability. We need a more extensive **data** set to firmly establish the correct interpretation of CV Vel's line-profile variability.