All Tables

• Table 1: Temporally and spatially averaged atmospheric stratification of the 3D solar surface convection simulation used for the 3D spectral line formation presented here: temperature, density, gas pressure, electron pressure and vertical velocity (positive velocities inward) as well as their rms-scatter. The spatial averaging has been performed over surfaces of the same continuum optical depths at 500 nm. Note that the original 3D model extends significantly above and below the optical depths for which the mean structure has been interpolated to and tabulated. We emphasize that it is not possible to explain all 3D effects by a comparison of such an averaged 3D model with existing 1D models due to the absence of atmospheric inhomogeneities.
• Table 2: The computed non-LTE abundance corrections for the three different model atmospheres. The departures from LTE have been estimated using MULTI3D (Botnen 1997; Asplund et al. 2003) for the 3D case and with MULTI (Carlsson 1986) for the 1D model atmospheres, in all cases using the same 23-level model atom.
• Table 3: The derived solar oxygen abundance as indicated by forbidden [O  I] and permitted O  I lines. The results for the O  I lines include the non-LTE abundance corrections presented in Table 2 which have been computed specifically for the three different model atmospheres.
• Table 4: The derived solar oxygen abundance as indicated by forbidden [O  I], permitted O  I lines, OH vibration-rotation line and OH pure rotation lines. The results for the O  I lines include the non-LTE abundance corrections presented in Table 2. The quoted uncertainties only reflect the line-to-line scatter for the different types of O diagnostics while no doubt the total error is dominated by systematic errors.