Abstract
A summary is given of (1) the theory of helium shell flashes in asymptotic giant branch stars and (2) the effect of helium shell flashes on the evolution of post asymptotic giant branch stars. In particular, the manner in which the shell flash wind (SFW) scenario accounts for the observed division of white dwarfs into two basic groups (those with nearly pure hydrogen atmospheres and those with nearly pure helium atmospheres) is described.
Supported in part by the U.S. National Science Foundation Grant AST 84–13371
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Iben, I. (1987). Helium Shell Flashes and their Consequences. In: Kwok, S., Pottasch, S.R. (eds) Late Stages of Stellar Evolution. Astrophysics and Space Science Library, vol 132. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3813-7_30
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