Abstract
The variation of the visible and ultraviolet fluxes of Be stars, as compared with their values during a non-emission phase of the star, is studied as a function of the emission intensity in the Ha and H lines. A correlation is found between the line emission intensities and the continuum flux in the visible range, but it seems that this correlation does not exist with the ultraviolet flux. However, some Be stars with a shell spectrum show a deficiency in the ultraviolet flux.
