Table 1: Galactic O-star sample: Stellar and wind parameters adopted ($M_{\rm v}$) and derived using FASTWIND. $T_{\rm eff}$ in kK, $R_{\ast }$ in ${R_{\odot }}$, $V_{\rm r}$sini and $v_{\rm\infty }$ in km s-1, $M_{\ast }$ in ${M_{\odot }}$, L in ${L_{\odot }}$, ${\dot M}$ in 10-6  ${M_{\odot }}$/yr (terminal velocities $v_{\rm\infty }$ from Paper I). HD 93129A and HD 303308 have recently been detected as binary systems but they are treated here as single stars (see text). Bold face numbers denote $\beta $-values which could be derived with high precision from emission profiles. Stars with absorption profiles were fitted with an assumed value of $\beta = 0.80$. $R_{\rm old}$ is the stellar radius resulting from our new models which was calculated by means of the "old'' $M_{\rm v}$ values from Paper I (not tabulated here).
Star Sp.Type $M_{\rm v}$ $T_{\rm eff}$ $\log g$ $\log g_{\rm true}^{2)}$ $R_{\ast }$ $Y_{\rm He}$ $V_{\rm r}$sini $v_{\rm\infty }$ $\log L$ $M_{\ast }$ ${\dot M}$ $\beta $ $R_{\rm old}$
HD 93129A1) O2 If* -6.74 42.5 3.70 3.71 (22.5) 0.10 130 3200 (6.17) (94.8) (26.30) $\bf0.80$ (21.4)
HD 93128 O3 V ((f)) -5.24 46.5 4.00 4.01 10.4 0.10 100 3100 5.66 39.8 2.64 0.853) 10.2
HD 93250 O3 V ((f)) -6.14 46.0 3.95 3.96 15.9 0.10 130 3250 6.01 83.3 3.45 0.903) 17.6
HD 66811 O4 I(f) -6.32 39.0 3.55 3.59 19.4 0.20 220 2250 5.90 53.9 8.80 $\bf0.90$ 16.8
HD 3033081) O4 V ((f+)) -5.29 41.0 3.90 3.91 (11.5) 0.075 120 3100 (5.53) (39.0) (1.63) 0.80 (12.6)
HD 14947 O5 If+ -5.94 37.5 3.45 3.48 16.8 0.20 140 2350 5.70 30.7 8.52 $\bf0.95 $ 18.1
HD 15558 O5 III(f) -6.27 41.0 3.80 3.81 18.2 0.10 150 2800 5.93 78.7 5.58 0.80 19.4
HD 193682 O5 III(f) -5.55 40.0 3.60 3.65 13.1 0.20 200 2800 5.60 27.9 1.73 0.80 12.3
HD 15629 O5 V ((f)) -5.50 40.5 3.70 3.71 12.8 0.08 90 3200 5.60 30.4 1.28 0.80 12.8
HD 210839 O6 I(n) fp -6.40 36.0 3.55 3.58 21.1 0.10 200 2250 5.83 62.2 6.85 $\bf 1.00 $ 20.2
HD 190864 O6.5 III(f) -5.29 37.0 3.55 3.57 12.3 0.15 105 2500 5.41 20.3 1.39 0.80 14.2
HD 192639 O7 Ib (f) -6.10 35.0 3.45 3.47 18.7 0.20 125 2150 5.68 37.5 6.32 $\bf0.90$ 19.6
HD 193514 O7 Ib (f) -6.15 34.5 3.30 3.32 19.3 0.10 105 2200 5.68 28.2 3.48 0.80 19.7
HD 24912 O7.5 III(n)((f)) -5.50 35.0 3.50 3.56 14.0 0.15 220 2450 5.42 26.1 1.08 0.80 11.6
HD 203064 O7.5 III:n ((f)) -5.74 34.5 3.50 3.60 15.7 0.10 300 2550 5.50 35.9 1.41 0.80 14.1
HD 217086 O7 V n -4.50 36.0 3.50 3.72 8.6 0.15 350 2550 5.05 14.2 $\le$0.23 0.80 10.4
HD 13268 ON8 V -4.77 33.0 3.25 3.48 10.3 0.25 300 2150 5.05 11.7 $\le$0.26 0.80 11.4
HD 210809 O9 Iab -6.20 31.5 3.10 3.12 21.2 0.14 100 2100 5.60 21.7 5.30 $\bf0.90$ 21.2
HD 207198 O9 Ib -5.80 33.0 3.45 3.46 16.6 0.12 80 2150 5.47 29.0 1.79 0.80 14.5
HD 30614 O9.5 Ia -7.00 29.0 2.97 2.99 32.5 0.10 100 1550 5.83 37.6 6.04 $\bf 1.15 $ 21.5
HD 209975 O9.5 Ib -6.41 32.0 3.20 3.22 22.9 0.10 100 2050 5.69 31.4 2.15 0.80 16.5
HD 18409 O9.7 Ib -5.58 30.0 2.95 3.04 16.3 0.14 150 1750 5.29 10.6 1.02 0.853) 15.7
HD 191423 O9 III:n* -5.24 32.5 3.35 3.60 12.9 0.20 400 1150 5.23 24.6 $\le$0.41 0.80 12.7
HD 149757 O9 V -4.35 32.0 3.65 3.85 8.9 0.17 400 1550 4.87 20.2 $\le$0.18 0.80 8.2
1) Component of binary system.
2) $\log g$ including centrifugal correction (see text).
3) Denotes those absorption profiles for which there are indications that $\beta $ differs from 0.80 (see text).

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