May 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984stin...8434352b&link_type=abstract
Presented at the IAU Colloq. on Cepheid Variables, Toronto, 29 May 1984
Physics
Cepheid Variables, Stellar Evolution, Stellar Models, Abundance, Binary Stars, Chemical Composition, Convection, Hertzsprung-Russell Diagram, Metallicity, Nuclear Reactions, Opacity, Star Clusters, Stars, Stellar Atmospheres, Stellar Luminosity, Stellar Mass, Stellar Rotation
Scientific paper
The phases of stellar evolution relevant to Cepheid variables of both types I and II are reviewed. Type I Cepheids arise as a result of normal post-main sequence evolutionary behavior of many stars in the intermediate to massive range of stellar masses. In contrast, type II Cepheids generally originate from low-mass stars of low metallicity which are undergoing post core helium-burning evolution. Despite great progress in the past two decades, uncertainties still remain in such areas as how to best model convective overshoot, semiconvection, stellar atmospheres, rotation, and binary evolution as well as uncertainties in important physical parameters such as the nuclear reaction rates, opacity, and mass loss rates. The potential effect of these uncertainties on stellar evolution models is discussed. Finally, comparisons between theoretical predictions and observations of Cepheid variables are presented for a number of cases. The results of these comparisons show both areas of agreement and disagreement.
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