The NaI, MgI, AlI, KI, SrII and BaII spectral line formation in stellar atmospheres of various Tef, 0.0 < log g < 4.5 and -4.0 < [M/H] < 0.5 was studied using models by Kurucz (1994). NLTE abundance corrections for the strongest spectral lines were obtained as functions of Tef, log g and [M/H]. As a rule NLTE effects increase with decreasing [M/H] and must be taken into account in chemical abundance determinations for metal deficient atmospheres.
IAU Joint Discussion
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