Table 1
Thirty-four elements included and their abundances.
| Element | log ɛ(a) | Element | log ɛ(a) | Element | log ɛ(a) |
|---|---|---|---|---|---|
| H | 12.00 | Al | 6.45 | Mn | 5.43 |
| He | 10.93 | Si | 7.51 | Fe | 7.50 |
| Li | −0.30(b) | P | 5.41 | Co | 4.99 |
| Be | 1.38 | S | 7.12 | Ni | 6.22 |
| B | 2.70 | Cl | 5.50 | Cu | 4.19 |
| C | 8.43(c) | Ar | 6.40 | Zn | 4.56 |
| N | 7.83 | K | 5.03 | Rb | 2.52(d) |
| O | 8.69 | Ca | 6.34 | Sr | 2.87(d) |
| F | 4.48(e) | Sc | 3.15 | Zr | 2.58 (d) |
| Ne | 7.93 | Ti | 4.95 | Ba | 2.18(d) |
| Na | 6.24 | V | 3.93 | ||
| Mg | 7.60 | Cr | 5.64 | ||
Notes. (a) Abundance defined as log ɛ(X) = 12 + log(X/H). Abundances are solar from Asplund et al. (2009) unless otherwise stated. (b) Abia et al. (1993). (c) The abundance of C in S-type and carbon stars is increased over the solar value to have C/O of 1.0 and 1.4, respectively. (d) The abundances of the s-process elements Rb, Sr, Zr, and Ba are increased over the solar values by 0.36, 1.01, 0.88, and 0.89 dex, respectively, in S-type stars (Abia & Wallerstein 1998) and by 0.26, 0.46, 0.67, and 0.51 dex, respectively, in carbon stars (Abia et al. 2002). (e) Abia et al. (2015).
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