HOW THIN B[E] SUPERGIANT DISKS CAN BE

We investigate the shape of the envelope around B [e] Mass flux superg iant stars using a model developed by Stee & Araujo (1994) for Be star s. We obtain mass loss rates (M) over dot between 5.5.10(-7) and 6.2.1 0(-6) M.yr(-1) depending on mass flux variation from polar to equatori al regions. We find that winds from B[e] stars can be so dense that th ey become optically thick in the continuum, masking the photosphere of the central star. For mass loss rates larger than 10(-5)M.yr(-1) it i s not possible to see the stellar photosphere even for pole-on B[e] st ars. Using a two-component wind model driven by optically thin lines i n the equatorial regions and optically thick lines in the polar region s, we obtain a relation between the geometry of the envelope and the t otal mass loss. We also put limits on the inclination angle (i) beyond which the stellar photosphere is masked. Finally, this study seems to discard ''wind-compressed disks'' (WCD) models as a possible senario for B[e] supergiant envelopes.