  We study the formation of O I and OH spectral lines in three-dimensional
hydrodynamic models of the solar photosphere. The line source function of the O
I 777 nm triplet is allowed to depart from local thermodynamic equilibrium
(LTE), within the two-level-atom approximation. Comparison with results from 1D
models show that the 3D models alleviate, but do not remove, the discrepancy
between the oxygen abundances reported from non-LTE work on the 777 nm triplet
and from the [O I] 630 nm and OH lines. Results for the latter two could imply
that the solar oxygen abundance is below 8.8 (lg(H) = 12). If this is
confirmed, the discrepancy between theory and observation for the 777 nm
triplet lines might fall within the range of errors in equivalent width
measurements and f-values. The line source function of the 777 nm triplet in
the 1.5D approximation is shown to differ insignificantly from the full 3D
non-LTE result.
