Abstract
We discuss oxygen abundances derived from (O ) λ6300 and the O triplet in stars spanning a wide range in chromo- spheric activity level, and show that these two indicators yield increasingly discrepant results with higher chromospheric/coronal activity measures. While the forbidden and permitted lines give fairly consistent results for solar-type disk dwarfs, spuriously high O triplet abundances are observed in young Hyades and Pleiades stars, as well as in individual components of RS CVn bi- naries (up to 1.8 dex). The distinct behaviour of the (O )-based abundances which consistently remain near-solar suggests that this phenomenon mostly results from large departures from LTE affecting the O triplet at high activity level that are currently unaccounted for, but also possibly from a failure to adequately model the atmospheres of K-type stars. These results suggest that some caution should be exercised when interpreting oxygen abundances in active binaries or young open cluster stars.
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