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Table 5

Parameters of HMXBs that appear in Figs. 3 and 4.

Binary Sp. Type log (LL) Teff [K] R* [R] M[M] D [R] LX [erg s−1] [M yr−1] tX Reference
IGR J00370+6122 (a),(b) B1Ib 4.91 24 000 16.5 10 36 (c) 2.5 × 1035 1.4 × 10−8 0.04 67, 68
2S 0114+650 (a) B1Iae 5.61 24 000 37 16 56 1.1 × 1036 1.6 × 10−7 0.24 1, 2, 37
Vela X-1 (a) B0Ia 5.49 25 500 28.4 20.2 50 3.5 × 1036 1.3 × 10−7 0.19 5, 56, 69
IGR J11215-5952 (b) B0.5Ia 5.73 24 700 40 29 80 (c) 3 × 1036 2.7 × 10−7 0.35 19, 20
1E 1145.1-6141 (a) B2Iae 5.12 19 500 32 14 63 1.1 × 1036 3.9 × 10−8 0.11 70, 71
GX 301-2 (a) B1.5Iae 5.67 18 100 70 43 180 2 × 1037 4.7 × 10−7 0.73 72, 73, 74
OAO 1657-415 B3Ia 4.95 20 000 24.8 14.3 50.3 3 × 1036 1.8 × 10−8 0.05 75, 76
IGR J18029-2016 B1Ib 5.14 25 000 19.8 20.2 33.1 2 × 1036 3.7 × 10−8 0.05 10, 29
IGR J18483-0311 (b) B0.5Ia 5.57 24 600 33.8 33 96 3.7 × 1035 1.6 × 10−7 0.24 14, 15, 42

Notes. Stellar parameters were taken from the listed references, except for the mass-loss rates, for which we used the fits from Krtička et al. (2021), neglecting clumping, and for the optical depth parameters, which were calculated from Eq. (10) using the fits for the mass-loss rates and terminal velocities from Krtička et al. (2021). (a)Some alternative designations: IGR J00370+6122 (BD+6073), 2S 0114+650 (V662 Cas), Vela X-1 (GP Vel, HD 77581), 1E 1145.1-6141 (V830 Cen), and GX 301-2 (BP Cru). (b)Supergiant fast X-ray transient (Lutovinov et al. 2013; Walter et al. 2015; Giménez-García et al. 2015). (c)Periastron distance.

References.(1) Reig et al. (1996); (2) Farrell et al. (2008); (5) Watanabe et al. (2006); (10) Mason et al. (2011); (14) Romano et al. (2010); (15) Rahoui & Chaty (2008); (19) Romano et al. (2007); (20) Lorenzo et al. (2014); (29) Hill et al. (2005); (37) Hall et al. (2000); (42) Searle et al. (2008); (56) Giménez-García et al. (2016); (67) Grunhut et al. (2014); (68) González-Galán et al. (2014); (69) Sander et al. (2018); (70) Ferrigno et al. (2008); (71) Hutchings et al. (1987); (72) Kaper et al. (2006); (73) Ikhsanov & Finger (2012); (74) Servillat et al. (2014); (75) Mason et al. (2012); (76) Chakrabarty et al. (2002).

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