Search

We calculate the evolution of a large and a medium mass star through the core H and He burning stages using the most recent OPAL opacities, both with and without a moderate amount of convective overshooting. The inclusion of the overshooting produces appreciable changes in the evolutionary track on the H-R diagram, in the durations of the central H and He burning phases and in the location of the H burning shell. In the medium mass case, the central temperature-density depends sensitively on whether or not overshooting is included.