The theory of radiatively-induced warps in accretion discs is applied to the discs of Be stars. It is found that these discs may develop warps in their inner regions, although once the warp amplitude is large enough then the interaction between the disc and fast radiatively-driven wind will determine its evolution. The warping is shown to be more important for later than earlier B stars. Although the interaction of the fast-wind with the disc will limit the amplitude of the warp, it cannot drive the warp radially outwards, and so the radial evolution of the warp depends on the dominant advective process within the disc. Typical timescales associated with growing modes are shown to be short, of the order of days-weeks, although these are not likely to be the timescales inferred from observations of line-profile variations which are much longer, of the order of years.