Abstract
AbstractPermitted OI, forbidden [OI], electronic AΣ − XП UV OH and vib-rot IR OH lines often infer different oxygen abundances for cool stars. Which species should one use to determine the oxygen abundance in cool stars and how does one reconcile the different results for different species? Although there are uncertainties and systematic differences in the molecular gf values used by different authors, the main reason for the different results lies in the 1-D model atmosphere analyses that are used.
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