Abstract
A previous comparison of thermodynamical quantities, computed in the chemical and physical pictures, revealed a remarkable agreement in the H and He ionization zones of the Sun, despite the radically different treatment of bound states in the two formalisms. This agreement was due to an unexpectedly dominating (classical) Coulomb pressure term. New comparisons, for higher temperatures and densities, and for a representative solar mixture (H, He and 0), have demonstrated substantial differences in the 0-ionization fractions. Also, the thermodynamic quantities reflect these differences to a degree that is within reach of helioseismology. Key words: EQUATION OF STATE - STARS: INTERIOR
