Abstract
ABSTRACT The main properties of the evolution of intermediate- and high-mass stars are reviewed, focusing on a few issues tightly related to the interpretation of population I Cepheid stars. The classical results of stellar evolution theory are given for the main evolutionary phases (main sequence, core He-burning, and later) all over the H-R diagram, putting into evidence the various points of disagreement with current observational data. The models incorporating the effect of convective overshoot are discussed, and a study on the rich young cluster NGC 1866 in the Large Magellanic Cloud is presented in which the models are compared with the observational data. Arguments are given to favor the adoption of models with convective overshoot instead of the classical ones. The topics of the mass discrepancy and number frequency-period distribution of Cepheid stars are then discussed in light of models with convective overshoot, arguing that these latter can better account for the observational data.
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