Ionization Equilibrium Equation of State. V. Twenty-Two Element Mixtures at Stellar Temperatures and Densities.

Abstract

The ionization equilibrium equation of state for a mixture of twenty-two elements has been calculate for two groups of temperatures and densities. The first group, given in tabular form, is the profile of a adopted photospheric model. The second group, given in graphical form, is a published profile of the su In the first group, three different H-He ratios are assumed, namely, 12.5, 20, and S. The two extreir ratios yield differences in the ratios of singly ionized to neutral metal atoms of about 20 per cent. In t second group of calculations, large variations in the mean molecular weight and - I occur in tt envelope. The variations of d /dr throughout the envelope and core give deeper insight into the proble of stellar stability.