A method for describing the continuum emission of a rapidly rotating star is derived. Explicit results for a model star of assumed initial spectral type B3V are included. Assumptions are made which, the author feels, do not remove the results too far from the realm of physical reality. Detailed calculations imply that a variation in color with angle of inclination exists for hot stars rotating near the breakup velocity. The effect becomes more significant as one approaches the far ultraviolet. The results of rotation upon the observed total flux from a star are also discussed. In addition some calculations are included which give insight into the behavior of the Balmer and Lyman lumps for a rapidly rotating star.