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Abstract

Oxygen is the most abundant “metal” element in stars and in the cosmos. But determining oxygen abundances in stars has proven challenging, because of the shortage of detectable atomic oxygen lines in their optical spectra as well as observational and theoretical complications with these lines (e.g., blends, three-dimensional, non-LTE). Nonetheless, Ting et al. were recently able to demonstrate that oxygen abundances can be determined from low-resolution (R ≃ 2000) optical spectra. Here, we investigate the physical processes that enable such a measurement for cool stars, such as K-giants. We show that the strongest spectral diagnostics of oxygen come from the CNO atomic-molecular network but are manifested in spectral features that do not involve oxygen. In the outer atmosphere layers, most of the carbon is locked up in CO, and changes to the oxygen abundance directly affect the abundances of all other carbon-bearing molecules, thereby changing the strength of CH, CN, and C₂ features across the optical spectrum. In deeper atmosphere layers, most of the carbon is in atomic form, and any change in the oxygen abundance has little effect on the other carbon-bearing molecules. The key physical effect enabling such oxygen abundance measurements is that spectral features in the optical arise from both the CO-dominant and the atomic carbon-dominant regions, providing non-degenerate constraints on both C and O. Beyond the case at hand, the results show that physically sound abundances measurements need not be limited to those elements that have observable lines themselves.