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Fig. 9


Evolution of the surface abundances of Li, Fe, and Ca as a function of Teff for two models with turbulence and two with mass loss identified in the figure. The chosen scale emphasizes the behavior on the subgiant and bottom of the giant branch. All models start (pre-main-sequence) to the right of the upper horizontal line and evolve to the left until they reach the main sequence at Teff ~ 6100 K. Then, diffusion starts being effective and the Li abundance, for instance, is reduced by 0.2 to 0.4 dex as the star approaches turnoff, at Teff ~ 6600 K. The models then move to the subgiant and giant branches where dilution further reduces the surface Li abundance by a factor of ~10. For Ca and Fe the radiative acceleration complicates the surface abundance evolution in the mass loss cases.

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