Abstract:
We deduce the density, pressure, and temperature profiles in the solar convective envelope by solving the basic equations for mass conservation and the hydrostatic equilibrium with the imposition of the helioseismologically determined sound-speed profile and equation of state. These profiles are required to match with the structure of the radiative core, which is also determined with the imposition of the sound speed profile. The depth of the convection zone and the helium abundance are obtained as a part of the solutions.
