Mass loss from cool stars

Abstract

Optical and UV spectroscopic diagnostics which provide constraints on theoretical models of mass-loss and mass motions in cool-star atmospheres are discussed. The use of X-ray and UV data for exploring the relationship between mass loss and stellar coronae, studying the characteristics of cool stellar winds, and modeling the mass-loss process in the cool half of the color-magnitude diagram is described. Solar observations which can be validly applied in generalized models of the complex interactions between a stellar magnetic field and plasma in a high gravity star are examined. Computational methods are defined for parameterizing mass-loss rates and deriving mass-loss rates of single evolved stars and binary systems. The effects of stellar mass loss on globular clusters are investigated.