A New Method of Automatic Computation of Stellar Evolution.

A method is described for obtaining time sequences of stellar models describing evolutionary changes This method is a modified version of an earlier one described by Henyey, lets, Bo'hm, LeLevier, and Lev6e (1959). The modifications involve the evaluation of all quantities at the same discrete points. The technique provides for coupling the interior integrations to those for model atmospheres based on mixinglength theory. The scope of the formalism is such as to provide for a wide range of calculations for spherically symmetric configurations in hydrostatic equilibrium.