Table A.1
Elements, mass fractions Xm, and ions used for the PoWRHD models in this worka.
| Element | Xm | Ions |
|---|---|---|
| He | (0.99) | I, II, III |
| Cb | (5.0 ∙ 10−5 for WR1) | I, II, III, IV, V, VI |
| (1.0 ∙ 10−5 for WR6, WR7, WR37) | ||
| (2.0 ∙ 10−5 for WR18) | ||
| (4.0 ∙ 10−4 for WR58) | ||
| Nb | (1.5 ∙ 10−2 for WR7) | I, II, III, IV, V |
| (1.0 ∙ 10−2 for rest) | ||
| O | (1.0 ∙ 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 | (6.9 ∙ 10−4) | I, II, III, IV |
| Al | (5.3 ∙ 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 | (1.6 ∙ 10−3) | II, III, IV, V, VI, VII |
Notes. (a)C, N, and O abundances are typical values for WN stars, values also adopted in the public PoWR WN grids (Todt et al. 2015). The remainder of the element abundances are the solar values derived in Asplund et al. (2009) and Scott et al. (2015a,b). (b)Depending on the star, adaptations to C and N abundances are made in order to improve spectral fits.
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