Motions of selected variable stars in the CaMD, highlighted by segments connecting successive absolute G magnitudes and G_BP − G_RP measurements in time with the same colour for the same source. Preferential directions and amplitudes of magnitude and colour variations can be inferred as a function of variability type (α² Canum Venaticorum, Be-type and γ Cassiopeiae, cataclysmic, classical and type-II Cepheid, δ Scuti and SX Phoenicis, eclipsing binary, long period, and RR Lyrae), as labelled in the figure. For clarity of visualisation, the selection of eclipsing binaries (and partially other types) was adjusted to minimise the overlap with other types. Selection criteria of all sources represented in colour or grey are the same as in Fig. 3. Additional conditions are described in the text. An animated version of this figure is available online.