Table 5
Parameters of HMXBs that appear in Figs. 3 and 4.
Binary | Sp. Type | log (L∕L⊙) | Teff [K] | R* [R⊙] | M[M⊙] | D [R⊙] | LX [erg s−1] | Ṁ [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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