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Table 10.
Comparison of the abundances (logarithmic mass fractions) derived for CD–31°4800 to the typical composition of the He-cores of RGB stars (of different mass MHe−core), coming from progenitors of different initial masses (MZAMS) and a metallicity of z = 0.01 (as computed by Miller Bertolami 2016).
| C | N | O | Ne | |
|---|---|---|---|---|
| CD−31 4800 | −4.14 ±0.16 | −2.38 ±0.11 | −4.22 ±0.13 | −2.74 ±0.12 |
| RGB cores | ||||
| MHe−core(MZAMS) | C | N | O | Ne |
| 0.20 M⊙ (1 M⊙) | −4.30 | −2.22 | −3.13 | −3.01 |
| 0.45 M⊙ (1 M⊙) | −4.20 | −2.20 | −3.39 | −3.01 |
| 0.20 M⊙ (1.5 M⊙) | −4.17 | −2.19 | −3.53 | −3.01 |
| 0.45 M⊙ (1.5 M⊙) | −4.13 | −2.19 | −3.69 | −3.01 |
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