Table 5
Summary of the NLTE results obtained in this analysis with our 3D model, and with the four different 1D models we used.
| Species | 3D | ⟨ 3D ⟩ | HM | marcs | miss | 3D−HM | 3D−⟨ 3D ⟩ | Recommended | Meteoritic | |
|
|
||||||||||
| log ϵNa | Na i | 6.21 ± 0.04 | 6.23 | 6.27 | 6.19 | 6.25 | −0.05 | −0.02 | 6.21 ± 0.04 | 6.27 ± 0.02 |
| log ϵMg | Mg i | 7.60 ± 0.04 | 7.61 | 7.64 | 7.56 | 7.63 | −0.04 | −0.01 | ||
| Mg ii | 7.58 ± 0.05 | 7.63 | 7.60 | 7.52 | 7.64 | −0.02 | −0.05 | |||
| Mg all | 7.59 ± 0.04 | 7.62 | 7.63 | 7.55 | 7.64 | −0.03 | −0.03 | 7.59 ± 0.04 | 7.53 ± 0.01 | |
| log ϵAl | Al i | 6.43 ± 0.04 | 6.45 | 6.48 | 6.40 | 6.47 | −0.05 | −0.02 | 6.43 ± 0.04 | 6.43 ± 0.01 |
| log ϵSi | Si i | 7.51 ± 0.03 | 7.50 | 7.52 | 7.44 | 7.53 | −0.01 | +0.01 | ||
| Si ii | 7.54 ± 0.04 | 7.58 | 7.55 | 7.47 | 7.60 | −0.02 | −0.04 | |||
| Si all | 7.51 ± 0.03 | 7.51 | 7.53 | 7.45 | 7.53 | −0.01 | 0.00 | 7.51 ± 0.03 | 7.51 ± 0.01 | |
| log ϵP | P i | 5.41 ± 0.03 | 5.43 | 5.42 | 5.38 | 5.45 | −0.01 | −0.01 | 5.41 ± 0.03 | 5.43 ± 0.04 |
| log ϵS | S i | 7.12 ± 0.03 | 7.14 | 7.12 | 7.06 | 7.15 | 0.00 | −0.02 | 7.12 ± 0.03 | 7.15 ± 0.02 |
| log ϵK | K i | 5.04 ± 0.05 | 5.06 | 5.11 | 5.02 | 5.09 | −0.06 | −0.02 | 5.04 ± 0.05 | 5.08 ± 0.02 |
| log ϵCa | Ca i | 6.32 ± 0.03 | 6.31 | 6.34 | 6.26 | 6.30 | −0.02 | +0.01 | ||
| Ca ii | 6.32 ± 0.04 | 6.34 | 6.33 | 6.28 | 6.36 | −0.02 | −0.03 | |||
| Ca all | 6.32 ± 0.03 | 6.32 | 6.34 | 6.26 | 6.31 | −0.02 | 0.00 | 6.32 ± 0.03 | 6.29 ± 0.02 | |
Notes. The uncertainties given for the 3D results are the total errors, including statistical and systematic contributions, calculated as described in Sect. 3. For comparison, we also give the mean abundance difference between the 3D and 1D HM models, and between the 3D and ⟨ 3D ⟩ (mean 3D) model. Note that because all means were computed using abundances accurate to three decimal places, entries in Cols. 8 and 9 differ in some cases from the differences between the entries in Cols. 3–5. We also give our final recommended abundance and the meteoritic values (Lodders et al. 2009, normalised to the silicon abundance determined in Paper I).
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