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Effects of line-blocking on the non-LTE Fe I spectral line formation

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Table 1. Stellar parameters for which the  model atmospheres used in this paper were computed
Table 2. Fe abundance corrections ∆ log  Fe = (log  Fe ) non−LTE − (log  Fe ) LTE for our sample stars
Fig. 3. Non-LTE Fe abundance corrections for the metal-poor stars HD 140283’s (top) and G64-12’s (bottom)  model atmospheres
Table 3. Fe non-LTE abundance corrections for our sample stars estimated from weak Fe  lines in the visible and near UV

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