2007ApJ...660..712S

We present oxygen abundances of dwarfs in the young open cluster IC 4665 deduced from the O I λ7774 triplet lines and of dwarfs in the open cluster Pleiades derived from the [O I] λ6300 forbidden line. Stellar parameters and oxygen abundances were derived using the spectroscopic synthesis tool SME (Spectroscopy Made Easy). We find a dramatic increase in the upper boundary of the O I triplet abundances with decreasing temperature in the dwarfs of IC 4665, consistent with the trend found by Schuler et al. in the open clusters Pleiades and M34 and to a less extent in the cool dwarfs of the Hyades by Schuler et al. and UMa by King & Schuler. By contrast, oxygen abundances derived from the [O I] λ6300 forbidden line for stars in the Pleiades and the Hyades from Schuler et al. are constant within the errors. Possible mechanisms that may lead a varying oxygen triplet line abundance are examined, including systematic errors in the stellar parameter determinations, the NLTE effects, surface activities, and granulation. The age-related stellar surface activities (especially the chromospheric activities) are suggested by our analysis to be responsible for the large spreads of oxygen triplet line abundances.