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Table 5

Parameters of binaries with non-degenerate components.

Binary Sp. Type log (L/L⊙) Teff R M Ṁ ν∞ tX a LX Reference
[K] [R⊙] [M⊙] [M⊙ yr-1] [km s-1] [R⊙] [erg s-1]
HR 8281 O6.5V 5.7 41 200 13.9 40.2 2.0 × 10-6 2290 3.6 40 2.3 × 1032 1, 2, 3
O9Va 5.02 34 900 8.9 22.4 9.7 × 10-8 2400
HD 152219 O9.5III 5.07 31 900 11.2 26.2 8.0 × 10-8 2320 0.2 37.1 8 × 1030 4
B1Va 3.74 21 800 5.2 10.3 3.4 × 10-10 2250
HD 47129 O8I 5.35 33 500 14.1 54. 2.0 × 10-7 2980 0.4 128.5 8.34 × 1032 5, 30
O7.5III 5.09 33 000 10.8 56. 9.0 × 10-8 3560 0.2
HR 6187 O3V 5.78 44 500 13.14 63 2.9 × 10-6 3090 3.9 38.0 3.2 × 1033 1, 6, 7, 8
O5.5Va 5.28 39 000 9.54 40. 3.0 × 10-7 3100
HR 6736 O3.5V 5.75 43 850 13.1c 55 2.6 × 10-6 2860 6.9 4100 1.2 × 1033 1, 9
O5V 5.5 40 850 11.2c 36 8.1 × 10-7 2560 2.8
V712 Car O3I 6.06 43 000 19.3 82.7 5.4 × 10-6 2720 2.8 53 7.5 × 1033 10, 11
O3I 6.06 43 000 19.3 81.9 5.4 × 10-6 2700 2.8
HR 65 O9III 5.2 32 000c 13 15 1.5 × 10-7 1490 0.3 32 7.2 × 1032 12, 13
O9III 4.83 32 000c 8.5 21 2.7 × 10-8 2430 0.0
HR 5664 O7V 5.27 37 500 10.2 21.6 2.9 × 10-7 2090 0.9 33.8 6.9 × 1031 1, 14
O9.5Vb 4.64 33 000 6.4 12.4 1.7 × 10-8 2140 0.0
HR 8406 O8.5III 5.11 32 000 11.7 16.9 9.7 × 10-8 1750 0.2 25.5 7.1 × 1031 1, 15
O9.5Va 4.69 28 000 9.4 6.7 2.2 × 10-8 1230
HD 93206A O9.7I 5.7 32 000 23 40 1.0 × 10-6 1780 2.0 116 3.4 × 1032 16, 29
B2Va 3.7 20 000 5.9 10 2.3 × 10-10 2080
HD 93206B O8III 5.3 32 600 14 14 2.3 × 10-7 1310 0.6 49 1.2 × 1032 16, 29
O9V 4.9 32 500 8.9 28 5.6 × 10-8 2750 0.1
V1007 Sco O7.5III 5.4 34 000 14.47 27.24 3.7 × 10-7 1950 0.5 51.7 4.4 × 1032 17, 18
O7III 5.5 34 350 15.99 27.88 5.9 × 10-7 1810 0.9
HR 1931 O9.5V 4.64 32 600 6.6c 19 1.8 × 10-8 2650 0.1 375 2.1 × 1032 1, 19, 31
B0Vb 4.45 30 600c 6.0c 15.4 2.6 × 10-9 2520 0.0
HR 6535 O6V 5.26 39 000c 9.4 32 2.9 × 10-7 2750 0.8 56.4 5.2 × 1032 1, 20, 21, 22
O7V 5.17 37 000c 9.4 32 1.9 × 10-7 2790 0.5
HR 1899 O9III 4.81 32 000c 8.3 23 2.5 × 10-8 2580 0.1 80 7.4 × 1032 1, 21, 23, 24
B0.5Vb 4.19 28 000c 5.3 13 1.8 × 10-9 2480 0.0
HR 1852 O9.5II 5.15 31 000c 13 11.2 7.8 × 10-8 1250 0.3 44 6.5 × 1032 1, 21, 25, 26
B0.5IIIb 4.2 29 000c 5 5.6 1.5 × 10-9 1640 0.0
V918 Sco O7.5I 5.9 35 100 24.3 57 2.7 × 10-6 2000 3.1 91 5.2 × 1032 1, 27
O9.7I 5.79 30 500 28.1 37 1.5 × 10-6 1430 0.7
HR 7767 O8.5III 5.25 32 500 13.4c 23 1.9 × 10-7 1900 0.7 620 8.9 × 1031 1, 28
B2.5Vb 3.29 20 000 3.7c 9 3.5 × 10-11 2500 0.0
DH Cep O5.5V 5.37 44 000 8.31 29.4 4.5 × 10-7 2720 0.9 26.4 5.4 × 1033 12, 32
O6.5Vb 5.27 43 000 7.76 25.0 2.9 × 10-7 2620 0.5
V1034 Sco O9V 4.78 33 200 7.45 16.8 3.3 × 10-8 2310 0.1 22.65 3.2 × 1031 33, 34
B1Va 3.87 26 200 4.18 9.4 5.8 × 10-10 2390
V1294 Sco O9V 5.1 34 000 10.3 24.5 1.4 × 10-7 2320 0.4 42.8 6.9 × 1031 35
O9.7V 4.71 31 200 7.8 18.2 2.4 × 10-8 2370 0.0
HD 93205 O3V 6.18 49 000 17.2c 45 1.8 × 10-5 1130 60.8 56.3 3.4 × 1033 36
O8Va 5.11 36 500 9.0c 20 1.4 × 10-7 2200

Notes. Stellar parameters are taken from literature except for the mass-loss rate, for which we used fits of Krtička & Kubát (2012) and Krtička (2014). Alternative designations: HR 8281 (HD 206267), HD 152219 (V1292 Sco), HD 47129 (V640 Mon, HR 2422, and Plaskett star), HR 6187 (HD 150136), HR 6736 (9 Sgr, HD 164794), V712 Car (WR 20a), HR 65 (AO Cas, HD 1337), HR 5664 (δ Cir, HD 135240), HR 8406 (14 Cep, LZ Cep, HD 209481), HD 93206 (QZ Car), V1007 Sco (HD 152248), HR 1931 (σ Ori, HD 37468), HR 6535 (V1036 Sco, HD 159176), HR 1899 (ι Ori A, HD 37043), HR 1852 (δ Ori, HD 36486), V918 Sco (HR 6164, HD 149404), HR 7767 (HD 193322), and HD 93205 (V560 Car).

(a)

The primary wind reaches the secondary surface (D2<R2).

(b)

The wind parameters lie in the forbidden area.

(c)

Derived from the effective temperature or spectral type using the expressions of Harmanec (1988) for main-sequence B stars and Martins et al. (2005a) for others.

Reference. (1) Berghöfer et al. (1997); (2) Burkholder et al. (1997); (3) Stickland (1995); (4) Sana et al. (2006a); (5) Linder et al. (2006); (6) Mahy et al. (2012); (7) Sana et al. (2013); (8) Sanchez-Bermudez et al. (2013); (9) Rauw et al. (2012); (10) Rauw et al. (2005); (11) Montes et al. (2013); (12) Chlebowski et al. (1989); (13) Sahade & Brandi (1991); (14) Penny et al. (2001); (15) Mahy et al. (2011); (16) Parkin et al. (2011); (17) Sana et al. (2004); (18) Mayer et al. (2008); (19) Simón-Díaz et al. (2011); (20) Pachoulakis (1996); (21) Gies (2003); (22) Chlebowski & Garmany (1991); (23) Marchenko et al. (2000); (24) Bagnuolo et al. (2001); (25) Harvin et al. (2002); (26) Mayer et al. (2010); (27) Rauw et al. (2001); (28) ten Brummelaar et al. (2011); (29) Leung et al. (1979); (30) Linder et al. (2008); (31) Najarro et al. (2011); (32) Sturm & Simon (1994); (33) Sana et al. (2005); (34) Bouzid et al. (2005); (35) Sana et al. (2008); (36) Antokhina et al. (2000).

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