Abstract
Using isentropic and homogeneous stellar models the final stages of stellar evolution are discussed. These primitive models are a natural generalization of polytropic models to cases of complex equations of state. The equations of state used in the present work include the effects of radiation, quantum degeneracy, relativistic electrons and pairs, and of a Fe-He transition. A limiting mass-entropy relation is discussed. This relation is a direct generalization of Chandrasekhar's limiting mass for white dwarfs, and is useful for obtaining a general picture of the evolutionary tracks at late stages. Tracks of central conditions on thep, T plane are calculated for isentropic models and the occurrence of various instabilities is discussed.
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