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Context. White dwarfs can be used to study the structure and evolution of theGalaxy by analysing their luminosity function and initial mass function. Amongthem, the very cool white dwarfs provide the information for the early ages ofeach population. Because white dwarfs are intrinsically faint only the nearby(about 20 pc) sample is reasonably complete. The Gaia space mission willdrastically increase the sample of known white dwarfs through its 5-6 yearssurvey of the whole sky up to magnitude V = 20-25.  Aims. We provide a characterisation of Gaia photometry for white dwarfs tobetter prepare for the analysis of the scientific output of the mission.Transformations between some of the most common photometric systems and Gaiapassbands are derived. We also give estimates of the number of white dwarfs ofthe different galactic populations that will be observed.  Methods. Using synthetic spectral energy distributions and the most recentGaia transmission curves, we computed colours of three different types of whitedwarfs (pure hydrogen, pure helium, and mixed composition with H/He= 0.1). Withthese colours we derived transformations to other common photometric systems(Johnson-Cousins, Sloan Digital Sky Survey, and 2MASS). We also present numbersof white dwarfs predicted to be observed by Gaia.  Results. We provide relationships and colour-colour diagrams among differentphotometric systems to allow the prediction and/or study of the Gaia whitedwarf colours. We also include estimates of the number of sources expected inevery galactic population and with a maximum parallax error. Gaia will increasethe sample of known white dwarfs tenfold to about 200 000. Gaia will be able toobserve thousands of very cool white dwarfs for the first time, which willgreatly improve our understanding of these stars and early phases of starformation in our Galaxy.