We have followed the evolution of stellar models of 1 and 1·2 M⊙ from a non-degenerate configuration to the stages where degeneracy becomes important and eventually causes the star to become a white dwarf. By detailed computer calculation using an evolution program kindly lent to us by Schwarzschild and Härm, we have obtained evolution sequences of stars of the mentioned masses with a core composition of 80% O, 10% Ne and 10% Mg and a thin outer envelope of He (10–6 of total mass) under the assumption of energy loss due to photons alone, and also under the assumption of losses due to photons plus neutrinos.