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A FORTRAN code which computes synthetic light and colour curves of active, spotted stars has been developed. The main feature of this code is its ability to model simultaneously the V light curve and the (V-R)_{c}, (V-I)_{c} and (V-K) colour data. It also uses new effective temperature-colour and Barnes-Evans-like calibrations, temperature and gravity-dependent limb-darkening coefficients and different effective surface gravities for the spotted and unspotted photosphere. The code allows for two-component spots, i.e., spots with umbral and penumbral components. Various problematic spot configuratins were investigated, taking us to the conclusion that, in order to be able to differentiate spots with various thermal structures (umbrae, penumbrae, faculae) or polar spots from equatorial bands, the modelling of the infrared colours, especially (V-I)c and (V-K), is needed.