  Apart from recent progress in Gamma Dor stars, identifying modes in rapidly
rotating stars is a formidable challenge due to the lack of simple, easily
identifiable frequency patterns. As a result, it is necessary to look to
observational methods for identifying modes. Two popular techniques are
spectroscopic mode identification based on line profile variations (LPVs) and
photometric mode identification based on amplitude ratios and phase differences
between multiple photometric bands. In this respect, the BRITE constellation is
particularly interesting as it provides space-based multi-colour photometry.
The present contribution describes the latest developments in obtaining
theoretical predictions for amplitude ratios and phase differences for
pulsation modes in rapidly rotating stars. These developments are based on full
2D non-adiabatic pulsation calculations, using models from the ESTER code, the
only code to treat in a self-consistent way the thermal equilibrium of rapidly
rotating stars. These predictions are then specifically applied to the BRITE
photometric bands to explore the prospects of identifying modes based on BRITE
observations.
