Table 3
Measured photospheric elemental abundances for the components of LL Aqr, derived from our disentangled HARPS and CORALIE spectra.
| A | Species | Star A | Lines | [X/H]A | Star B | Lines | [X/H]B | log ϵ⊙ | ||
|
|
||||||||||
| 3 | Li i | 2.88 ± 0.10 | 1 | 1.65 ± 0.10 | 1 | 1.05 ± 0.10 | ||||
| 6 | C i | 8.55 ± 0.07 | 4 | 0.12 ± 0.09 | 8.57 ± 0.06 | 9 | 0.14 ± 0.08 | 8.43 ± 0.05 | ||
| 11 | Na i | 6.27 ± 0.07 | 4 | 0.03 ± 0.08 | 6.28 ± 0.05 | 8 | 0.04 ± 0.07 | 6.24 ± 0.04 | ||
| 12 | Mg i | 7.56 ± 0.07 | 2 | − 0.01 ± 0.08 | 7.56 ± 0.06 | 5 | − 0.04 ± 0.07 | 7.60 ± 0.04 | ||
| 14 | Si i | 7.55 ± 0.05 | 13 | 0.04 ± 0.06 | 7.60 ± 0.03 | 14 | 0.09 ± 0.04 | 7.51 ± 0.03 | ||
| 20 | Ca i | 6.38 ± 0.05 | 18 | 0.04 ± 0.06 | 6.38 ± 0.06 | 21 | 0.04 ± 0.07 | 6.34 ± 0.04 | ||
| 21 | Sc ii | 3.20 ± 0.04 | 5 | 0.05 ± 0.05 | 3.16 ± 0.03 | 9 | 0.01 ± 0.05 | 3.15 ± 0.04 | ||
| 22 | Ti i | 4.93 ± 0.04 | 33 | − 0.02 ± 0.06 | 4.97 ± 0.06 | 37 | 0.02 ± 0.08 | 4.95 ± 0.05 | ||
| 23 | V i | 3.96 ± 0.05 | 15 | 0.03 ± 0.09 | 3.96 ± 0.06 | 13 | 0.03 ± 0.10 | 3.93 ± 0.08 | ||
| 24 | Cr i | 5.65 ± 0.04 | 11 | 0.01 ± 0.05 | 5.62 ± 0.08 | 29 | − 0.02 ± 0.09 | 5.64 ± 0.08 | ||
| 25 | Mn i | 5.43 ± 0.04 | 7 | 0.00 ± 0.06 | 5.46 ± 0.08 | 5 | 0.03 ± 0.10 | 5.43 ± 0.05 | ||
| 26 | Fe i | 7.54 ± 0.03 | 229 | 0.04 ± 0.05 | 7.55 ± 0.07 | 229 | 0.05 ± 0.08 | 7.50 ± 0.04 | ||
| 26 | Fe ii | 7.53 ± 0.03 | 16 | 0.03 ± 0.05 | 7.54 ± 0.06 | 16 | 0.04 ± 0.08 | 7.50 ± 0.04 | ||
| 27 | Co i | 4.90 ± 0.05 | 6 | − 0.09 ± 0.08 | 4.99 ± 0.07 | 22 | 0.00 ± 0.10 | 4.99 ± 0.07 | ||
| 28 | Ni i | 6.25 ± 0.04 | 81 | 0.03 ± 0.06 | 6.27 ± 0.08 | 88 | 0.05 ± 0.09 | 6.22 ± 0.04 | ||
| 29 | Cu | 4.24 ± 0.12 | 2 | 0.05 ± 0.13 | 4.22 ± 0.10 | 4 | 0.03 ± 0.11 | 4.19 ± 0.04 | ||
| 39 | Y ii | 2.22 ± 0.08 | 6 | 0.01 ± 0.09 | 2.18 ± 0.03 | 10 | − 0.03 ± 0.06 | 2.21 ± 0.05 | ||
| 56 | Ba ii | 2.02 ± 0.07 | 2 | 0.16 ± 0.11 | 2.29 ± 0.07 | 1 | 0.11 ± 0.12 | 2.18 ± 0.09 | ||
Notes. Columns list the atomic number, element, and degree of ionisation, and then for each component the logarithmic value of the elemental abundance on the usual scale in which log n(H) = 12, the number of spectral lines measured, and the logarithmic abundance relative to the Sun of element X with respect to hydrogen. The last column gives the reference photospheric solar values from Asplund et al. (2009).
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