Abstract
SummaryA review of diffusion in F, A and B stars is presented. The basic equations are introduced in a simple and approximate way. Meridional circulation, magnetic fields, surface gravity and age are all factors that contribute to variations in anomalies for stars of a given effective temperature. Detailed calculations for each of these effects, as well as of radiation forces in the atmosphere, are needed before the required detailed comparison between theory and observations can be made for individual stars. When it is made this comparison should put strong constraints on stellar atmosphere or envelope models. At the present level of uncertainty no difficulty between theory and observations appears definitely established.
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