Li and Na abundances for TO and SGB stars in NGC 6397 (data from Paper I, with improved non-LTE derivation). The initial [Na/Fe], shown on the abscissa, has been estimated by correcting A(Na) for atomic diffusion by + 0.2 dex and assuming [Fe/H] = −2.1 for all stars. The red bullets represent turn-off stars and the blue stars subgiants. Superimposed are the theoretical predictions for the chemical composition of the matter out of which second generation low-mass stars are expected to form in the WFRMS scenario. The tracks shown correspond to the cases of 20 M⊙ and 120 M⊙ polluter stars (dashed and full lines, respectively) assuming different values (0.2, 0.4, 0.6, 0.8) for the minimum dilution coefficient. See text for more details.
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