Table 1.
Stellar, wind and clumping parameters for models in Sect. 4.
| Name | Teff [K] | log g [cgs] | R*/R⊙ | log Ṁ (M⊙/yr) | v∞ (km s−1) | β | Lx/LBol | fcl | fic | fvel | h∞/R* |
|---|---|---|---|---|---|---|---|---|---|---|---|
| O1 smooth | 40 000 | 3.6 | 19.0 | −5.22 | 2200 | 1.0 | 0 | 1.0 | – | – | – |
| O1 thin | 40 000 | 3.6 | 19.0 | −5.22 | 2200 | 1.0 | 0 | 10.0 | – | – | – |
| O1 thick | 40 000 | 3.6 | 19.0 | −5.22 | 2200 | 1.0 | 0 | 10.0 | 0.01 | 0.5 | 1.0 |
| O2 smooth | 35 000 | 3.45 | 20.0 | −5.22 | 2000 | 1.0 | 0 | 1.0 | – | – | – |
| O2 thin | 35 000 | 3.45 | 20.0 | −5.22 | 2000 | 1.0 | 0 | 10.0 | – | – | – |
| O2 thick | 35 000 | 3.45 | 20.0 | −5.22 | 2000 | 1.0 | 0 | 10.0 | 0.01 | 0.5 | 1.0 |
| O3 smooth | 30 000 | 3.2 | 22.0 | −5.22 | 1600 | 1.0 | 0 | 1.0 | – | – | – |
| O3 thin | 30 000 | 3.2 | 22.0 | −5.22 | 1600 | 1.0 | 0 | 10.0 | – | – | – |
| O3 thick | 30 000 | 3.2 | 22.0 | −5.22 | 1600 | 1.0 | 0 | 10.0 | 0.01 | 0.5 | 1.0 |
| B7 smooth | 12 000 | 1.8 | 100.0 | −5.52 | 400 | 1.0 | 0 | 1.0 | – | – | – |
| B7 thin | 12 000 | 1.8 | 100.0 | −5.52 | 400 | 1.0 | 0 | 10.0 | – | – | – |
| B7 thick | 12 000 | 1.8 | 100.0 | −5.52 | 400 | 1.0 | 0 | 10.0 | 0.01 | 0.5 | 1.0 |
| ∼ζ Pup thin | 40 000 | 3.63 | 18.9 | −5.74 | 2250 | 0.9 | ∼10−7 | 20.0 | – | – | – |
| ∼ζ Pup thick1 | 40 000 | 3.63 | 18.9 | −5.74 | 2250 | 0.9 | ∼10−7 | 20.0 | 0.01 | 0.5 | 1.0 |
| ∼ζ Pup thick2 | 40 000 | 3.63 | 18.9 | −5.74 | 2250 | 0.9 | ∼10−7 | 20.0 | 0 | 0.5 | 1.0 |
Notes. For simplicity, all models here assume clumping starts at v/v∞ = 0.05, increases linearly until the value given in table below is reached at v/v∞ = 0.1, and then stays constant throughout the rest of the wind. All models further assume a velocity-stretch porosity law h/h∞ = v/v∞ (see text) and solar metallicity. However, for the ζ Pup like models the He and CNO abundances are modified from the solar scale according to nHe/nH = 0.16, and AC = 6.73, AN = 8.7, AO = 8.48 on the standard abundance scale AX = log10(nx/nH) + 12.
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