Table 2
Stellar and wind parameters as adopted/derived in the present analysis.
| Star | Sp. type | Mv | Teff | log g | R∗ | YHe | log (L/L⊙) | vsini | vmacro | v∞ | Ṁ | β | fv | CL2 | v turb | log Dmom |
|
|
||||||||||||||||
| Cyg OB2 7 | O3 If∗ | –5.911 | 45.1 | 3.75 | 14.7 | 0.13 | 5.91 | 95 | 65 | 3100 | 1.2 | 1.05 | 0.03 | 100 | 10 | 28.95 |
| HD 66811 | O4 I(n)f | –6.322 | 40.0 | 3.63 | 18.9 | 0.14 | 5.92 | 215 | 95 | 2250 | 2.1 | 0.90 | 0.03 | 180 | 10 | 29.11 |
| Cyg OB2 8C | O5 If | –5.611 | 37.4 | 3.61 | 14.3 | 0.10 | 5.56 | 175 | 90 | 2800 | 2.0 | 1.30 | 0.10 | 550 | 20 | 29.13 |
| Cyg OB2 8A | O5.5 I(f) | –6.911 | 37.6 | 3.52 | 26.9 | 0.10 | 6.12 | 110 | 80 | 2700 | 3.4 | 1.10 | 0.01 | 500 | 10 | 29.48 |
| HD 30614 | O9.5 Ia | –7.002 | 28.9 | 3.01 | 32.0 | 0.13 | 5.81 | 100 | 75 | 1550 | 0.50 | 1.60 | 0.01 | 25 | 17.5 | 28.44 |
| HD 37128 | B0 Ia | –6.993 | 26.3 | 2.90 | 34.1 | 0.13 | 5.70 | 55 | 60 | 1820 | 0.46 | 1.60 | 0.03 | 30 | 15 | 28.49 |
|
|
||||||||||||||||
| HD 217086 | O7 Vn | –4.502 | 36.8 | 3.83 | 8.56 | 0.1 | 5.08 | 350 | 80 | 2510 | 0.028 | 1.2 | 0.10 | 30 | 10 | 27.11 |
| HD 36861 | O8 III((f)) | –5.394 | 34.5 | 3.70 | 13.5 | 0.11 | 5.37 | 45 | 80 | 2175 | 0.28 | 1.3 | 1.0 | – | 7.5 | 28.15 |
| HD 76341 | O9 Ib | –6.294 | 32.2 | 3.66 | 21.2 | 0.1 | 5.64 | 63 | 80 | 1520 | 0.065 | 1.2 | 1.0 | – | 7.5 | 27.46 |
| HD 37468 | O9.5 V | –3.904 | 32.6 | 4.19 | 7.1 | 0.1 | 4.71 | 35 | 100 | 1500 | 0.0002 | 0.8 | 1.0 | – | 5 | 24.70 |
Notes. Teff in kK, R∗ in R⊙, all velocities in km s-1, Ṁ in 10-6 M⊙/yr and modified wind-momentum rate, Dmom = Ṁv∞(R ⋆ /R⊙)0.5, in cgs. The gravitational acceleration, log g, is the effective one, i.e., not corrected for centrifugal forces. The volume filling factor, fv, corresponds to the parameter CL1 in Eq. (1) and describes the maximum degree of clumping reached in the stellar wind. However, since our analysis bases on stratified clumping factors, the usual scaling of 
does not or only approximately apply in most cases. CL2 (km s-1) indicates the onset of clumping in the wind. The horizontal line separates objects displaying significant wind emission in Hα, i.e., dense winds (see Sect. 4), from objects with a pure absorption Hα profile, i.e., thin winds (Sect. 5).
References.
from the calibration provided by Martins et al. (2005a).
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