Evidence for a small, high-Z, iron-like solar core

The oscillation periods of nonradial g-modes in a recent numerical model of the sun are presented. The model was calculated using a coupled system of first-order nonlinear differential equations which describe stellar structure from the high-Z iron-like solar core to the surface. Theoretical eigenvalues for the oscillation modes were compared with recent observational data obtained from the Stanford Solar Observatory (SSO) and the Crimean Astrophysical Observatory (CAO), and the results are discussed in detail. Comparison with the analytical solutions of Tassoul (1980); Scuflaire (1974); and Robe (1968) showed good agreement for the g-mode calculations. The average period spacings for the l = 1 and 2 modes were in qualitative agreement with Osaki's (1975) calculations for high-Z core orders n with s = n + 1/2 - 1/4 less than 18. Additional evidence is presented to support the high-Z iron-like solar core hypothesis.