Seismic solar model: both of the radiative core and the convective envelope

Abstract

We determine the solar internal structure by solving the basic stellar structure equations with the imposition of the sound speed, which is inferred from helioseismology. As for the radiative core, all the four structure equations are solved with the boundary conditions set at the center and at the top of the radiative core. As for the convective envelope, we only have to solve the basic equations for mass conservation and hydrostatic equilibrium with the imposition of the sound-speed profile determined from helioseismology, as an intial value problem from the base of the convection zone. The helium abundance is obtained as a part of the solutions. The extent of the convection zone is also determined so that the temperature gradient matches the adiabatic gradient at the bottom of the zone, and the deduced depth is 0.718Rsolar.