Abstract
Abstract Winds of high-mass main sequence and highly evolved stars are probably driven primarily by radiation pressure acting on the wind gas (e.g. Lucy and Abbot 1993), while the sustained winds of low-mass and intermediate-ma1;1s highly evolved stars may be affected substantially by radiation pressure acting on dust (cf. Chapter 12). However, radiation pressure is incapable of inducing the high mass-loss rates of 10-9 M0 yr-1 to 10-4 M0 yr-1 characteristic of low-mass (;≲ 4 M0) young stellar objects (YSOs) in some phases of their evolution. The highest mass-loss rates are often associated with clearly defined bipolar flows (e.g. Bachiller 1996); some low-mass YSOs are also seen to possess jets and Herbig-Haro objects (cf. Chapter 10).
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