Seismic model of the solar convective envelope

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, we solve all the four structure equations and deduce the mass, luminosity, pressure, temperature, density, and hydrogen and helium abundances. We use the mass and the pressure at the top of the radiative core, obtained in this way, as the initial conditions for the equations governing the solar convective envelope, and determine the structure of the solar convective envelope by solving the basic equations for mass conservation and hydrostatic equilibrium with the imposition of the sound-speed profile determined from helioseismology and the equation of state. The solution is required to satisfy M(R.) = M.. 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 0.718R..