One might think that the most appropriate division of topics in a two volume book on stellar evolution physics would be the placement of all chapters describing the input physics required for the construction of stellar models in the first volume and the placement of all chapters describing stellar evolutionary models in the second volume. However, such a division disguises the fact that it is the operation of the input physics in stars that explains why they shine and evolve and that, therefore, both the input physics and the response of stars to the operation of this physics comprise the science of stellar evolution physics.

In preparing this book, after describing much of the input physics required for the construction of stellar models during early evolutionary stages, I constructed models in these early stages of evolution. Then, after describing some of the more complicated physical processes that play important roles during more advanced stages of evolution, I constructed models in these more advanced stages. The ordering of topics in the two volumes of this book reflects this chronological development.

After providing a general introduction to the observed properties of real stars and to the results of stellar evolution calculations, the first volume focusses on equations of state, energy generation by hydrogen-burning reactions, energy transport by radiation and convection, and on the elementary equations of stellar evolution and methods of solution.