Element Diffusion in the Solar Interior

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.

TeX document, 25 pages, for hardcopy with figures contact [email protected]. Institute for Advanced Study number AST 93/17

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• Revisiting the exoplanet radius valley with host stars from SWEET-Cat
• PLATO Hare-and-Hounds exercise: Asteroseismic model fitting of main-sequence solar-like pulsators
• 12 Bootis: the need for asteroseismic constraints
• Probing stellar cores from inversions of frequency separation ratios
• The SAPP pipeline for the determination of stellar abundances and atmospheric parameters of stars in the core program of the PLATO mission
• Variations of helioseismic parameters due to magnetic field generated by a flux transport model
• Asteroseismology of the DAV star R808