Orbital phase of the low-frequency total intensity (S_I) and circularly-polarised (S_V) emission for BF Lyn (top left), EV Dra (top right), Sig CrB (bottom left) and YY Gem (bottom right). The orbital phase for which our model predicts we should observe emission is shown as red-lines at arbitrary flux densities. For Stokes V we use red and blue to distinguish between the two polarisations. Sig CrB was observed in three independent 8 h epochs, while all other stellar systems were only observed in two independent epochs. The prediction for Sig CrB has been shifted 0.5 in phase, which corresponds with emission originating on the secondary, to show the good correspondence with the data. The polarity of the Stokes V prediction is arbitrary because we do not know which magnetic pole is pointed towards us. Therefore the prediction for the stars where we see emission from both poles (YY Gem and EV Dra) can be flipped in sign.