Do bipolar magnetic regions exist on the surfaces of early-type stars ?

The observations of relatively narrow absorption components of the UV resonance lines in the spectra of early-type stars are reviewed, and some new observational data are presented for ρ Leo (B1 Ib). It is suggested that the ejected parcels of gas which are required to form the discrete components seen in the spectra of many hot stars may be like the "magnetic clouds" observed by Burlaga and his associates in the solar wind at distances of 200 to 800 solar radii above the surface of the Sun. A discussion of the physical processes necessary to obtain these clouds leads to the conclusion that bipolar magnetic regions exist on the surfaces of hot stars.