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Table 3
LTE atmospheric abundances in programme stars with the error estimates based on the internal scattering from the number of analysed lines, n.
| Ion | VAS 20 | VAS 87 | Sun | ||
| log (N/Ntot) | n | log (N/Ntot) | n | log (N/Ntot) | |
|
|
|||||
| Li i | −8.55 ± 0.16 | 1 | −8.60 ± 0.10 | 1 | −10.99 |
| Na i | −5.83 ± 0.08 | 2 | −5.68: | 2 | −5.87 |
| Mg i | −4.63 ± 0.03 | 4 | −4.55 ± 0.12 | 4 | −4.44 |
| Si i | −4.58 ± 0.09 | 7 | −4.87 ± 0.14 | 5 | −4.53 |
| Si ii | −4.49: | 1 | −4.53 | ||
| Ca i | −5.64 ± 0.09 | 16 | −5.71 ± 0.14 | 10 | −5.70 |
| Sc ii | −8.97 ± 0.09 | 6 | −9.16: | 1 | −8.89 |
| Ti i | −7.00 ± 0.08 | 6 | −7.08 ± 0.15 | 3 | −7.09 |
| Ti ii | −7.03 ± 0.06 | 8 | −7.14 ± 0.13 | 6 | −7.09 |
| Cr i | −6.37 ± 0.17 | 15 | −6.39 ± 0.10 | 6 | −6.40 |
| Cr ii | −6.44 ± 0.14 | 8 | −6.06 ± 0.08 | 5 | −6.40 |
| Mn i | −6.62 ± 0.15 | 4 | −6.44 ± 0.14 | 5 | −6.61 |
| Fe i | −4.55 ± 0.10 | 127 | −4.63 ± 0.15 | 45 | −4.54 |
| Fe ii | −4.52 ± 0.08 | 17 | −4.58 ± 0.20 | 14 | −4.54 |
| Co i | −7.13: | 1 | −7.05 | ||
| Ni i | −5.77 ± 0.10 | 16 | −5.83 ± 0.08 | 8 | −5.82 |
| Cu i | −8.03: | 1 | −7.68: | 1 | −7.85 |
| Y ii | −9.94 ± 0.08 | 2 | −9.66 ± 0.03 | 2 | −9.83 |
| Ba ii | −9.29 ± 0.04 | 3 | −9.51 ± 0.05 | 2 | −9.86 |
Notes. For comparison purpose, the last column gives the abundances of the solar atmosphere calculated by Asplund et al. (2009).
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