On OH line formation and oxygen abundances in metal-poor stars
The formation of the UV OH spectral lines has been investigated for a range of stellar parameters in the light of 3D hydrodynamical model atmospheres. The low atmospheric temperatures encountered at low metallicities compared with the radiative equilibrium values enforced in classical 1D hydrostatic model atmospheres have a profound impact on the OH line strengths. As a consequence, the derived O abundances using 3D models are found to be systematically lower by more than 0.6 dex at [Fe/H]...[Show more]
|Collections||ANU Research Publications|
|Source:||Astronomy and Astrophysics|
|oh.pdf||1.13 MB||Adobe PDF|
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