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A chromosphere is a universal attribute of stars of spectral type later than~F5. Evolved (K and M) giants and supergiants (including the zeta Aurigaebinaries) show extended and highly turbulent chromospheres, which develop intoslow massive winds. The associated continuous mass loss has a significantimpact on stellar evolution, and thence on the chemical evolution of galaxies.Yet despite the fundamental importance of those winds in astrophysics, thequestion of their origin(s) remains unsolved. What sources heat a chromosphere?What is the role of the chromosphere in the formation of stellar winds? Thischapter provides a review of the observational requirements and theoreticalapproaches for modeling chromospheric heating and the acceleration of winds insingle cool, evolved stars and in eclipsing binary stars, including physicalmodels that have recently been proposed. It describes the successes that havebeen achieved so far by invoking acoustic and MHD waves to provide a physicaldescription of plasma heating and wind acceleration, and discusses thechallenges that still remain.

Atmospheric Heating and Wind Acceleration: Results for Cool Evolved Stars based on Proposed Processes