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Context: The prediction of stellar angular diameters from broadbandphotometry plays an important role for different applications. In particular,long-baseline interferometry, gravitational microlensing, extrasolar planettransits, and many other observing techniques require accurate predictions ofthe angular size of stars. These predictions are based on the surfacebrightness-colour (SBC) relations. Aims: Our goal is to calibrategeneral-purpose SBC relations using visible colours, the most commonlyavailable data for most stars. Methods: We compiled the existing long-baselineinterferometric observations of nearby dwarf and subgiant stars and thecorresponding broadband photometry in the Johnson B V and Cousins Rc Ic bands.We then adjusted polynomial SBC models to these data. Results: Due to thepresence of spectral features that depend on the effective temperature, the SBCrelations are usually not linear for visible colours. We present polynomialfits that can be employed with BVRcIc based colours to predict thelimb-darkened angular diameters (i.e. photospheric) of dwarf and subgiant starswith a typical accuracy of 5%. Conclusions: The derived polynomial relationsprovide a satisfactory approximation to the observed surface brightness ofnearby dwarfs and subgiants. For distant stars, the interstellar reddeningshould be taken into account, and will usually introduce an additionaluncertainty to the predicted angular diameters.

The angular sizes of dwarf stars and subgiants - Non-linear surface brightness relations in BVRcIc from interferometry