摘要：It has been suggested that Fe abundances of K dwarfs derived from Fe i and Fe ii lines show considerable discrepancies, and oxygen abundances determined from high-excitation O i 7771–5 triplet lines are appreciably overestimated (the problem becoming more serious toward lower Teff), which, however, has not yet been widely confirmed.With the aim of clarifying this issue, we spectroscopically determined the atmospheric parameters of 148 G–K dwarfs (Hyades cluster stars and field stars) by assuming the classical Fe i/Fe ii ionization equilibrium as usual, and determined their oxygen abundances by applying the non-local thermal equilibrium spectrum fitting analysis to O i 7771–5 lines.It turned out that the resulting parameters did not show any significant inconsistency with those determined by other methods (for example, the mean differences in Teff and $\mathrm{log}g$ from the well-determined solutions of Hyades dwarfs are mostly lesssim100 K and lesssim0.1 dex).Likewise, the oxygen abundances of Hyades stars are around [O/H] ~ +0.2 dex (consistent with the metallicity of this cluster) without exhibiting any systematic Teff-dependence.Accordingly, we conclude that parameters can be spectroscopically evaluated to a sufficient precision in the conventional manner (based on the Saha–Boltzmann equation for Fe i/Fe ii) and oxygen abundances can be reliably determined from the O i 7771–5 triplet for K dwarfs as far as stars of Teff gsim 4500 K are concerned.We suspect that previously reported strongly Teff-dependent discrepancies may have stemmed mainly from overestimation of weak-line strengths and/or improper Teff scale.
关键词：Stellar abundances;Stellar atmospheres;Fundamental parameters of stars;Late-type stars;Open star clusters
