Table A.2
Comparison of stellar and wind parameters as derived in the present analysis with results from previous investigations.
| Star | ref. | Teff | log g | R∗ | YHe | vsini | vmacro | v∞ | Ṁ | β | fv | log (L/L⊙) | log Qres | log Q | |
|
|
|||||||||||||||
| Cyg OB2 7 | t.w. | 45.1 | 3.75 | 14.7 | 0.13 | 95 | 65 | 3100 | 1.2 | 1.05 | 0.03 | 5.91 | –14.07 | –12.15 | |
| 3 | 45.5 | 3.71 | 14.6 | 0.30 | 105 | 3080 | 9.86 | 0.9 | 5.92 | –11.99 | |||||
| 6 | 45.8 | 3.94 | 14.4 | 0.21 | 105 | 3080 | 9.98 | 0.77 | 5.92 | –11.97 | |||||
| 7 | 44.0 | 3.71 | 14.6 | 0.10 | 145 | 3080 | 10.0 | 5.86 | –11.98 | ||||||
| 8 | 45.8 | 3.94 | 15.0 | 0.21 | 105 | 3080 | ≤ 4.0 | 0.9 | 0.2 | 5.95 | –12.05 | ||||
| HD 66811 | t.w. | 40.0 | 3.63 | 18.9 | 0.14 | 215 | 95 | 2250. | 2.1 | 0.90 | 0.03 | 5.92 | –13.66 | –11.86 | |
| 1 | 39.0 | 19.4 | 219 | 2250 | 0.44 | 0.5 | 5.90 | –14.35 | |||||||
| 4 | 39.2 | 3.65 | 17.5 | 0.20 | 203 | 2300 | 6.4 | 0.92 | 5.82 | –12.10 | |||||
| 5 | 39.0 | 3.59 | 19.4 | 0.20 | 220 | 2250 | 8.8 | 0.9 | 5.90 | –12.02 | |||||
| 7 | 39.0 | 3.59 | 19.4 | 0.17 | 220 | 2250 | 8.77 | 5.90 | –12.02 | ||||||
| 8 | 39.0 | 3.6 | 18.6 | 0.20 | 220 | 2250 | 4.2 | 0.70 | 0.2 | 5.86 | –11.96 | ||||
| Cyg OB2 8C | t.w. | 37.4 | 3.61 | 14.3 | 0.10 | 175 | 90 | 2800 | 2.0 | 1.30 | 0.10 | 5.56 | –13.75 | –12.10 | |
| 3 | 41.0 | 3.81 | 13.3 | 0.09 | 145 | 2650 | 2.25 | 0.9 | 5.65 | –12.47 | |||||
| 6 | 41.8 | 3.74 | 13.3 | 0.13 | 145 | 2650 | 3.37 | 0.85 | 5.69 | –12.29 | |||||
| 7 | 39.0 | 3.62 | 13.3 | 0.10 | 145 | 2650 | 2.0 | 5.57 | –12.52 | ||||||
| 8 | 41.8 | 3.81 | 15.6 | 0.13 | 145 | 2650 | ≤ 3.5 | 1.0 | 1.0 | 5.83 | –12.38 | ||||
| Cyg OB2 8A | t.w. | 37.6 | 3.52 | 26.9 | 0.10 | 110 | 80 | 2700 | 3.4 | 1.10 | 0.01 | 6.12 | –13.76 | –11.76 | |
| 3 | 38.5 | 3.51 | 27.9 | 0.10 | 95 | 2650 | 13.5 | 0.7 | 6.19 | –12.17 | |||||
| 6 | 38.2 | 3.57 | 25.6 | 0.14 | 130 | 2650 | 10.4 | 0.74 | 6.10 | –12.23 | |||||
| 7 | 37.0 | 3.41 | 27.9 | 0.10 | 95 | 2650 | 11.5 | 6.12 | –12.24 | ||||||
| 8 | 38.2 | 3.57 | 27.0 | 0.14 | 130 | 2650 | ≤ 8.0 | 0.74 | 0.40 | 6.15 | –12.18 | ||||
| HD 30614 | t.w. | 28.9 | 3.01 | 32.0 | 0.13 | 100 | 75 | 1550 | 0.50 | 1.60 | 0.01 | 5.81 | –14.19 | –12.34 | |
| 1 | 29.0 | 32.5 | 129 | 1550 | 0.037 | 1.0 | 5.83 | –15.32 | |||||||
| 4a | 31.0 | 3.19 | 24.9 | 0.10 | 100 | 1550 | 4.2 | 1.05 | 5.71 | –12.26 | |||||
| 5 | 29.0 | 2.99 | 32.5 | 0.10 | 100 | 1550 | 6.04 | 1.15 | 5.83 | –12.27 | |||||
| 7 | 29.0 | 2.88 | 32.5 | 0.20 | 100 | 1550 | 6.0 | 5.83 | –12.28 | ||||||
| 8b | 29.0 | 3.0 | 32.5 | 0.10 | 100 | 1550 | 2.95 | 1.15 | 0.38 | 5.83 | –12.37 | ||||
| HD 37128 | t.w. | 26.3 | 2.90 | 34.1 | 0.13 | 55 | 60 | 1820 | 0.46 | 1.60 | 0.03 | 5.70 | –14.39 | –12.77 | |
| 2 | 28.5 | 3.00 | 35.0 | 0.1 | 80 | 1600 | 2.40 | 1.25 | 5.86 | –12.74 | |||||
| 7 | ≤ 29.0 | 3.0 | 35.0 | 0.1 | 80 | 1600 | 5.25 | 5.89 | –12.40 | ||||||
|
|
|||||||||||||||
| HD 217086 | t.w. | 36.8 | 3.83 | 8.56 | 0.1 | 350 | 80 | 2510 | 0.028 | 1.2 | 0.10 | 5.08 | –15.28 | –13.55 | |
| 1 | 36.0 | 8.6 | 332 | 2550 | ≤ 0.00174 | 1.0 | 5.05 | –16.51 | |||||||
| 5 | 36.0 | 3.72 | 8.6 | 0.15 | 350 | 2550 | ≤ 0.23 | 0.8 | 5.05 | –13.15 | |||||
| 6 | 38.1 | 4.01 | 8.3 | 0.09 | 350 | 2550 | 0.21 | 1.27 | 5.12 | –13.17 | |||||
| 7 | 36.0 | 3.78 | 8.6 | 0.15 | 350 | 2550 | ≤ 0.09 | 5.05 | –13.56 | ||||||
| HD 36861 | t.w. | 34.5 | 3.70 | 13.5 | 0.11 | 45 | 80 | 2175 | 0.28 | 1.3 | 1.0 | 5.37 | –14.36 | –13.25 | |
| 1 | 33.6 | 15.1 | 74 | 2400 | 0.0013 | 0.7 | 5.42 | –16.83 | |||||||
| 4 | 33.6 | 3.56 | 17.2 | 0.1 | 66 | 2400 | 0.97 | 0.8 | 5.53 | –12.94 | |||||
| 8 | 33.6 | 3.56 | 14.4 | 0.10 | 66 | 2400 | ≤ 0.4 | 0.9 | 0.5 | 5.38 | –13.06 | ||||
| HD 76341 | t.w. | 32.2 | 3.66 | 21.2 | 0.1 | 63 | 80 | 1520 | 0.065 | 1.2 | 1.0 | 5.64 | –14.88 | –13.95 | |
| HD 37468 | t.w. | 32.6 | 4.19 | 7.1 | 0.1 | 35 | 100 | 1500 | 0.0002 | 0.8 | 1.0 | 4.71 | –16.90 | –15.74 | |
| 7c | 30.0 | 4.0 | 7.1 | 0.1 | 80 | 2300 | 0.0165 | 1.0 | 4.57 | –14.10 | |||||
Notes. Units as in Table 2; optical depth invariants, Q and Qres (see Eq. (A.1)), calculated with Ṁ in M⊙ yr-1, R∗ in R⊙ and v∞ in km s-1. fv values from this work as in Table 2, i.e., equal to CL1 (Eq. (1)). fv values from reference (8) (Puls et al. 2006) corresponding to the clumping factors within the innermost clumped region (“region 2”) extending between 1.1 ≤ r/R ⋆ ≤ 2 and assuming an unclumped outer wind. For reference (1) (Fullerton et al. 2006), the quoted results for Ṁ and log Qres include the product with the ionization fraction of Pv.
stellar radius and corresponding quantities scaled to the solution by (5, 7) to facilitate the comparison;
References. (1) Fullerton et al. (2006); (2) Kudritzki et al. (1999,unblanketed analysis); (3) Herrero et al. (2002); (4) Markova et al. (2004,based on stellar parameters calibrated to the results from optical NLTE analyses by Repolust et al. 2004; (5) Repolust et al. (2004); (6) Mokiem et al. (2005); (7) Repolust et al. (2005); (8) Puls et al. (2006).
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