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Article Contents
1 Introduction
2 3D hydrodynamical model atmospheres
3 Spectral line formation in 3D model atmospheres
4 3D LTE oxygen abundances derived from UV OH lines
5 Possible systematic errors affecting the 3D results
6 Comparing previous OH, O I and [O I] results
7 Concluding remarks
References

Copyright ESO 2001
Published by EDP Sciences