Abstract
After the main-sequence the evolution of stars begins to depend more and more on their initial mass. The discussion of post-main sequence evolution is therefore best split into different mass ranges. We begin with the intermediate mass range and the evolution through the second major burning phase, core helium burning. Typical representatives of this phase and mass range are the classical Cepheids.
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Kippenhahn, R., Weigert, A., Weiss, A. (2012). Evolution Through Helium Burning: Intermediate-Mass Stars. In: Stellar Structure and Evolution. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-30304-3_31
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DOI: https://doi.org/10.1007/978-3-642-30304-3_31
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