Table 4
Average abundances implied by Sc i, Sc ii, Ti i, Ti ii, V i, V ii, Cr i, Cr ii, Mn i, Fe i, Fe ii, Co i, Ni i and Ni ii lines.
| Species | 3D | ⟨ 3D ⟩ | HM | marcs | miss | 3D−HM | 3D−⟨ 3D ⟩ | Recommended | Meteoritic | |
|
|
||||||||||
| log ϵSc | Sc i | 3.14 ± 0.09 | 3.21 | 3.28 | 3.18 | 3.23 | −0.14 | −0.07 | 3.16 ± 0.04 | 3.05 ± 0.02 |
| Sc ii | 3.17 ± 0.04 | 3.16 | 3.19 | 3.14 | 3.19 | −0.02 | 0.01 | |||
| Sc all | 3.16 ± 0.04 | 3.18 | 3.22 | 3.15 | 3.21 | −0.07 | −0.03 | |||
| log ϵTi | Ti i | 4.88 ± 0.05 | 4.94 | 4.99 | 4.90 | 4.93 | −0.11 | −0.06 | 4.93 ± 0.04 | 4.91 ± 0.03 |
| Ti ii | 4.97 ± 0.04 | 4.94 | 4.97 | 4.91 | 4.97 | 0.00 | 0.02 | |||
| Ti all | 4.90 ± 0.04 | 4.94 | 4.99 | 4.90 | 4.94 | −0.08 | −0.04 | |||
| log ϵV | V i | 3.89 ± 0.08 | 3.99 | 4.07 | 3.96 | 4.00 | −0.18 | −0.10 | 3.89 ± 0.08 | 3.96 ± 0.02 |
| (V ii) | 4.00 ± 0.04 | 3.98 | 4.01 | 3.95 | 4.01 | −0.01 | 0.02 | |||
| log ϵCr | Cr i | 5.60 ± 0.04 | 5.62 | 5.66 | 5.57 | 5.63 | −0.06 | −0.02 | 5.62 ± 0.04 | 5.64 ± 0.01 |
| Cr ii | 5.65 ± 0.04 | 5.62 | 5.63 | 5.56 | 5.65 | +0.03 | 0.04 | |||
| Cr all | 5.62 ± 0.04 | 5.62 | 5.65 | 5.57 | 5.64 | −0.04 | −0.01 | |||
| log ϵMn | Mn i | 5.42 ± 0.04 | 5.43 | 5.47 | 5.37 | 5.42 | −0.04 | −0.00 | 5.42 ± 0.04 | 5.48 ± 0.01 |
| log ϵFe | Fe i | 7.45 ± 0.04 | 7.46 | 7.52 | 7.41 | 7.46 | −0.07 | −0.00 | 7.47 ± 0.04 | 7.45 ± 0.01 |
| Fe ii | 7.51 ± 0.04 | 7.46 | 7.46 | 7.42 | 7.49 | +0.05 | 0.05 | |||
| Fe all | 7.47 ± 0.04 | 7.46 | 7.50 | 7.41 | 7.47 | −0.03 | 0.01 | |||
| log ϵCo | Co i | 4.93 ± 0.05 | 4.96 | 4.99 | 4.92 | 4.96 | −0.06 | −0.03 | 4.93 ± 0.05 | 4.87 ± 0.01 |
| log ϵNi | Ni i | 6.20 ± 0.04 | 6.20 | 6.24 | 6.15 | 6.23 | −0.04 | 0.00 | 6.20 ± 0.04 | 6.20 ± 0.01 |
| (Ni ii) | 6.30 ± 0.10 | 6.23 | 6.24 | 6.19 | 6.26 | +0.06 | 0.08 | |||
Notes. Abundances are given as the weighted mean across all lines in the given list, taking into account NLTE corrections for Sc i, Sc ii, Ti i, V i, Cr i, Mn i, Fe i and Co i. V ii and Ni ii are shown in brackets because we do not consider these results reliable enough to include in our final adopted abundances. We also give our final recommended solar photospheric abundance of each element, compared with the abundance in CI chondritic meteorites (Lodders et al. 2009, normalised to the silicon abundance determined in Paper I). 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.
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