Abstract
Mass loss due to outflow is one factor introducing uncertainty into our understanding of the evolution of massive stars. There is a need of a theory, that would make it possible to take into account mass loss in the process of evolutionary computations in a self-consistent way. It is currently clear that the role of outflow is extremely important for stellar evolution, but quantitative conclusions about mass-loss rates remain uncertain. The evolution of stars with masses M ≥ 15 M⊙ is accompanied by mass loss at rates reaching 10–4-10–6 M⊙ yr–1. This strongly influences the evolution of such stars in the supergiant stage.
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