Optical light variability appears to be commonplace in Be stars, on time scales from days to decades, but the phenomenon has yet to be satisfactorily explained. Some possible causes include changes in 1) the star's photospheric temperature or radius, or 2) the envelope's opacity or continuous emission. To investigate the nature of the photometric variability in Be stars, we have been monitoring the FUV flux of selected objects with the ultraviolet spectrometers (UVS) on the Voyager 1 and 2 spacecrafts (cf. Broadfoot, et al. 1977, and Holberg, et al. 1982, respectively, for information on the instrumentation and calibration, and Drilling, et al. 1984 and Polidan, et al. 1987 for a discussion of data reduction techniques), and report the initial results from these observations in this paper.