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Table 3

Wind properties of the sample stars.

Star − Sp. type − log M˙$\[\dot{M}\]$ (M⊙ yr−1) v∞ (km s−1) β − ξmax (km s−1) f∞ − vcl (km s−1) log (L/LX) − TX (MK) vX (km s−1)
AzV 235 B0.2 Ia −6.17 1490 2.4 100 0.02 5 −6.8 1.0 700
AzV 215 BN0 Ia −6.44 1600 2.8 100 0.20 30 −7.3 1.0 100
AzV 488 B0.5 Iaw −6.07 1200 1.7 100 0.20 30 −7.4 1.0 700
AzV 104 B0.5 Ia −6.96 350 0.5 300 0.60 30 −8.9 0.5 400
AzV 242 B0.7 Iaw −6.39 900 1.8 200 0.20 30 −7.5 1.0 500
AzV 266 B0.7 Ia −6.92 985 1.8 147 0.10 30 −7.2 1.0 500
AzV 264 B1 Ia −6.82 820 1.8 120 0.20 30 −8.7 0.5 500
AzV 210 B1.5 Ia −6.66 810 2.5 100 1.00 30 −8.2 0.5 730
Sk 191 B1.5 Ia −6.02 490 2.8 60 0.80 400 −8.5 0.5 400
AzV 78 B1 Ia+ −5.82 520 3.0 90 0.75 30 −8.6 0.5 590
AzV 18 B2 Ia −6.66 350 1.5 60 1.00 30 −9.1 0.5 270
AzV 472 B2 Ia −7.52 190 1.3 150 0.60 30 −9.1 0.5 160
AzV 187 B3 Ia −7.22 450 2.2 60 0.30 30 −8.0 0.5 380
AzV 362 B3 Ia −6.92 200 2.5 60 0.10 30 −8.1 0.5 170
AzV 22 B3 Ia −7.15 197 3.7 25 0.10 30 −8.2 0.5 170
AzV 234 B2.5 Ib −7.74 140 2.2 60 1.00 30 −8.6 0.5 120
Sk 179 B3II −8.00 240 1.1 60 0.35 30 −8.3 0.5 200
AzV 343 B8 Iab −8.00 260 2.0 150 1.00 30 −8.2 0.5 250
Errors − 0.40 10% − − − − − − −

Notes. For AzV 235 we employed the clumping law introduced by Najarro et al. (2011), which uses two additional parameters to account for a decrease in the clumping factor in the outer wind. In our model, the two parameters are C3 = 300 km s−1 and C4 = 1.0.

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