B(e)-supergiants of the Magellanic Clouds.

Spectroscopic and photometric observations at the satellite UV, visual, and infrared wavelengths of 8 Magellanic Clouds dusty B[e]-supergiants are discussed. In spite of their high luminosity these stars show little or no photometric or spectroscopic variations. Apart from R 66 (B8 Ia) all stars are early B supergiants. The peculiar emission line spectra appear to be a consequence of unique wind characteristics. A two component stellar wind model, comprising a slow, dense, cool equatorial wind and a normal radiation driven wind in the polar region, can account for the observations. It is concluded that the known B[e]-stars of the Magellanic Clouds are massive (30 ⪉ M ⪉ 80 M_sun;) post-main sequence objects where stellar rotation plays an important role for the mass loss.