Table A.1
Elements, ions and their respective abundances in mass fractions Xm used in this work for the Z = Z⊙-sequencea,b.
| Element | Xm | Ions |
|---|---|---|
| H | (0.2) | I, II |
| He | (0.63) | I, II, III |
| N | (0.015) | I, II, III, IV, V |
| C | (1 · 10−4) | I, II, III, IV, V, VI |
| O | (1 · 10−4) | I, II, III, IV, V, VI |
| Ne | (1.3 · 10−3) | I, II, III, IV, V, VI, VII |
| Na | (2.7 · 10−5) | I, II, III, IV, V |
| Mg | (7.0 · 10−4) | I, II, III, IV |
| Al | (5.7 · 10−5) | I, II, III, IV, V |
| Si | (6.7 · 10−4) | I, II, III, IV, V, VI |
| P | (5.8 · 10−6) | II, III, IV, V, VI |
| S | (3.1 · 10−4) | I, II, III, IV, V, VI, VII |
| Cl | (8.2 · 10−6) | III, IV, V, VI, VII |
| Ar | (7.3 · 10−5) | I, II, III, IV, V, VI, VII, VIII |
| K | (3.1 · 10−6) | I, II, III, IV, V, VI, VII |
| Ca | (6.1 · 10−5) | II, III, IV, V, VI, VII, VIII |
| Fe | (1.4 · 10−3) | II, III, IV, V, VI, VII |
Notes. (a)Abundance values for CNO are adopted from the distribution typically found in WN stars and adopted in the public PoWR WN grids (e.g., Todt et al. 2015) (b)Other elements have been pulled from Asplund et al. (2009) and Scott et al. (2015a,b) with Fe reflecting the “iron group” from Sc to Ni, summarizing their abundances.
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