The star CoRoT102781750 reveals a puzzle, showing a very complex and altering variation in different `CoRoT colours. We established without doubt that more than a single star was situated within the CoRoT mask. Using a search for periodicity as a tool, our aim is to disentangle the composite light curve and identify the type of sources behind the variability. Both flux and magnitude light curves were used. Conversion was applied after a jump- and trend-filtering algorithm. We applied different types of period-finding techniques including MuFrAn and Period04. The amplitude and phase peculiarities obtained from the independent analysis of CoRoT r, g, and b colours and ground-based follow-up photometric observations ruled out the possibility of either a background monoperiodic or a Blazhko type RR Lyrae star being in the mask. The main target, an active star, shows at least two spotted areas that reveal a $P_rot = 8.8$ hours $(f_0 = 2.735$ c d$^{-1})$ mean rotation period. The evolution of the active regions helped to derive a period change of $dP/dt = 1.6cdot 10^{-6}$ (18 s over the run) and a differential rotation of $alpha = DeltaOmega/Omega = 0.0074$. The $0fm 015$ linear decrease and a local $0fm 005$ increase in the dominant periods amplitude are interpreted as a decay of the old spotted region and an appearance of a new one, respectively. A star that is detected only in the CoRoT b domain shows a $f_1 = 7.172$ c d$^{-1}$ pulsation connected to a $14fd 83$ periodicity via an equidistant triplet structure. The best explanation for our observation is a $beta$ Cep star with a corotating dust disk.
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