Predicted visible emitter area as a function of orbital phase for our targets that have measured inclinations. We have assumed a theoretical model for the emission geometry given by Melrose & Dulk (1982) with electron speed β = 0.2 as an estimate. The ‘step’-like variations between adjacent points are gridding artefacts. We have assumed that the observer’s line of sight always hits the northern magnetic hemisphere of the emitting star. Solid lines are for electrons travelling from the north magnetic pole to the south magnetic pole, dashed lines are for electrons travelling vice versa. Sincewe do not know if we are observing the northern or southern magnetic hemisphere, these definitions are interchangeable. BQ CVn, DM UMa, DG CVn and BD+334462 have been left out because we lacked the necessary parameters to make an accurate prediction (namely the semi-major axis for the first three star systems, and the inclination for the last one).