Abstract
Throughout the domain of the H-R diagram lie groupings of stars whose luminosity varies with time. These variable stars can be classified based on their observed properties into distinct types such as β Cephei stars, σ Cephei stars, and Miras, as well as many other categories. The underlying mechanism for the variability is generally felt to be due to four different causes: geometric effects, rotation, eruptive processes, and pulsation. In this review the focus will be on pulsation variables and how the theory of stellar evolution can be used to explain how the various regions of variability on the H-R diagram are populated. To this end a generalized discussion of the evolutionary behavior of a massive star, an intermediate-mass star, and a low-mass star will be presented.
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© 1987 Springer-Verlag
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Becker, S.A. (1987). The evolution of variable stars. In: Cox, A.N., Sparks, W.M., Starrfield, S.G. (eds) Stellar Pulsation. Lecture Notes in Physics, vol 274. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-17668-3_166
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DOI: https://doi.org/10.1007/3-540-17668-3_166
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