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Fig. 14.
Same as Fig. 11 for samples observed by Liu et al. (2014); in this case, Li data is NLTE. We show only their stars with −0.2 ≤ [Fe/H] ≤ 0.2 and compare with solar metallicity models including rotation and thermohaline mixing from Lagarde et al. (2012) computed for [Fe/H] = 0.
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