SIMBAD references

The rise of ultraviolet astronomy in the seventies and eighties of the last century has taught us that all hot luminous stars are blowing fierce winds into space with velocities of several thousand km.s^–1 and mass-loss rates of 10^–6 to 10^–4 M_☉.yr^–1. The mass-loss rates of the normal O, B, and A stars are well explained by radiation pressure due to spectral lines, including the observed bi-stability jumps near spectral types B1 and A0. However, several important observed wind features are not well understood: the presence of corotating spiral-like structures in the wind, the high densities of flat outflowing equatorial disks, and the high mass-loss rates of the Wolf-Rayet stars. I discuss the discovery and early ideas about winds from hot stars and the triumphs and failures of the radiation-driven wind theory.