Key points are not available for this paper at this time.
Results of a quantitative analysis of white-dwarf evolution are presented for models employing an accurate dense-plasma equation of state and incorporating a full treatment of partial ionization as well as convection in the envelope. Results are discussed in detail for a pure C-12 star of 1 solar mass. It is shown that the cooling curve and luminosity function deviate substantially from the behavior predicted by Mestel's (1952) cooling theory due to neutrino energy losses and Debye cooling, and that crystallization occurs when the dimensionless parameter Gamma attains a value of 160. Stellar lifetime is increased by almost a factor of three in the phase preceding Debye cooling due to the combined effect of increased heat capacity and the release of latent heat during crystallization. The theoretical results are found to be consistent with observational data. The possibility of observing such stars is evaluated.
Lamb et al. (Mon,) studied this question.