Revised solar photospheric abundances yield Z/X = 0.0187 with C, N, O at 8.46, 7.83, 8.69, preserving the solar modeling discrepancy and revealing a modest volatile-refractory offset from CI chondrites.
Element Diffusion in the Solar Interior
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abstract
We study the diffusion of helium and other heavy elements in the solar interior by solving exactly the set of flow equations developed by Burgers for a multi-component fluid, including the residual heat-flow terms. No approximation is made concerning the relative concentrations and no restriction is placed on the number of elements considered. We give improved diffusion velocities for hydrogen, helium, oxygen and iron, in the analytic form derived previously by Bahcall and Loeb. These expressions for the diffusion velocities are simple to program in stellar evolution codes and are expected to be accurate to $\sim 15\%$. Our complete treatment of element diffusion can be directly incorporated in a standard stellar evolution code by means of an exportable subroutine, but, for convenience, we also give simple analytical fits to our numerical results.
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The chemical make-up of the Sun: A 2020 vision
Revised solar photospheric abundances yield Z/X = 0.0187 with C, N, O at 8.46, 7.83, 8.69, preserving the solar modeling discrepancy and revealing a modest volatile-refractory offset from CI chondrites.