Structure Of The Sun's Core: Evolutional And Seismological Constraints

Introduction A variety of solar models (namely, models of stars having solar values of mass, radius, luminosity) is a subject of our study. The hydrogen profile in the star's interior is usually determined by course of the evolution, but we also consider models with arbitrary hydrogen profiles or diffusion profiles also. Applying additional restrictions on the model which follow from recent helioseismic results we consider the question of existence of the models. These restrictions are: 1) calibration of the surface helium abundance and the specific entropy in the convection zone (Vorontsov et al. 1991; Baturin, Vorontsov 1994; there are few results on the helium calibration but we used cited ones because they contain simultaneous determination of the helium and the entropy); 2) estimation of the convection zone depth (Christensen-Dalsgaard et al., 1991); 3) sound speed profile inferred from oscillation frequencies (Vorontsov, Shibahashi 1992)