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Table 5

Sample of analysed OB stars in this work and the initial set of stellar and wind parameters from the literature (‘ref’ column) used as input values in our simulations. log g indicates gravities without centrifugal correction.

Source Spec. type Teff log g R* YHe υ β d ref Alt. name
(kK) (R) (number) (km s−1) (10−6 M yr−1) (kpc)
HD 66811 O4 I (n)f 39.0 3.60 18.6 0.2 2250 0.9 4.2 0.46 8 ζ Pup
29.7 8.5 0.73 8
Cyg OB2#11 O5 If+ 36.5 3.62 23.6 0.1 2300 1.1 5.0 1.71 8
HD 210839 O6 I (n)f 36.0 3.55 23.3 0.1 2250 1.0 3.0 1.077 8 λ Cep
HD 152408 O8 Iafpe 33.0 3.20 30.0 0.2 955 2.1 8.4 1.68 7a
HD 151804 O8 Iab 32.8 3.25 35.0 0.1 1450 2.0 6.4 1.8 7a V973 Sco
HD 149404 O9 Ia 34.0 3.55 37.0 0.1 2450 1.3 1.95 1.3 9
HD 30614 O9.5 Ia 29.0 3.0 20.7 0.1 1550 1.15 1.5 0.8 8 α Cam

HD 37128 B0 Ia 27.0 2.9 24.0 0.2 910 1.5 2.5 0.363 2 ϵ Ori
HD 38771 B0.5 Ia 26.5 2.9 22.2 0.2 1525 1.5 0.9 0.4 2 κ Ori
HD 154090 B0.7 Ia 22.5 2.65 36.0 0.2 915 1.5 0.95 1.096 2 κ Sco
HD 193237 B1 Ia 16.7 2.0 97.14 0.3 195 2.5 5.4 1.7 7b P Cyg
HD 24398 B1 I 20.26 2.95 23.0 0.2 1295 1.5 0.23 0.28 11 ζ Per
HD 169454 B1.5 Ia+ 20.4 2.35 74.0 0.1 850 2.1 6.4 1.54 7a
HD 152236 B1.5 Ia+ 18.0 2.0 112.4 0.2 390 2.0 6.0 1.995 2 ζ1 Sco
HD 41117 B2 Ia 19.0 2.35 61.9 0.2 510 2.0 0.9 1.5 2 χ2 Ori
HD 194279 B2 Ia 19.0 2.3 44.7 0.2 550 2.5 1.05 1.202 2
HD 198478 B2.5 Ia+ 17.5 2.12 49.0 0.1–0.2 200....470 1.3 0.117.....0.407 0.83 4 55 Cyg
HD 80077 B2/B3 Iae 15.1 1.85 243.0 0.35 250 3.0 1.18 3.6 1, 3, 6
HD 53138 B3 Ia 15.5 2.05 65.0 0.2 865 2.0 0.36 1.096 2 o2 CMa
Cyg OB2#12 B3-4Ia 13.7 1.7 246.0 0.2 400 1.5 15.0 1.75 1

HD 24912 O7.5 III (n)((f)) 35.0 3.5 24.2 0.15 2450 0.9 2.3 0.854 8 ξ Per
HD 36861 O8 III((f)) 33.6 3.56 14.4 0.1 2400 0.9 0.4 0.5 8 λ Ori A
HD 37043 O9III 31.4 3.5 17.9 0.12 2300 0.9 0.8./0.25 0.5 8 ι Ori

HD 149757 O9.5 Vnn 32.0 3.65 8.9 0.17 1550 0.8 ≲0.18 0.154 10a,10b ζ Oph
HD 149438 B0.2 V 31.9 3.99 5.3 0.12 2400 0.8 ≲0.0614 0.167 6, 11 τ Sco

Notes. For HD 66811 (ζ Pup) we provide two entries, based on different distances (P06). References. [1] Clark et al. (2012); [2] Crowther et al. (2006); [3] Marco & Negueruela (2009); [4] Markova & Puls (2008); [5] Morel et al. (2004); [6] Mokiem et al. (2005); [7a] Najarro (1995); [7b] Najarro (priv. comm.); [8] Puls et al. (2006); [9] Raucq et al. (2016); [10a] Repolust et al. (2004); [10b] Repolust et al. (2005); [11] Simón-Díaz et al. (2006).

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