Abstract
Consistently with a trend observed in recent past triennial reports, progress in the theory of stellar atmospheres continues to be made in two different directions: (i) the traditional areas of continuum and line radiation transfer, line blanketing, atomic physics and atmospheric structures controlled by the joint conditions of radiative and hydrostatic equilibrium, and (ii) in areas of emerging interest such as oscillations, winds and mass loss, chromospheres, coronae and magnetic phenomena.
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