Table A.2
Parameters of the stellar atmosphere models calculated for the 50 M⊙ track with Z = 0.05 Z⊙ (Marchant et al. 2016).
| Model | MII 1 | MII 2 | MII 3 | MII 4 | MII 5 | |||
| a | b | a | b | a | b | |||
|
|
||||||||
| Spectral type | O3 V((f*)) | Of/WN | WN2.5 | WN2 | WN2 | |||
| age [106 yr] | 0.11 | 5.07 | 5.36 | 5.54 | 5.83 | |||
| T∗ [kK] | 50.4 | 66.5 | 70.3 | 100.0 | 150.0 | |||
| log L [L⊙] | 5.53 | 6.05 | 6.10 | 6.15 | 6.16 | |||
| M [M⊙] | 50.1 | 46.4 | 44.3 | 42.2 | 35.4 | |||
| R∗ [R⊙] | 7.7 | 8.0 | 7.6 | 4.0 | 1.8 | |||
| log Ṁ [M⊙/ yr] | –6.7 | –5.3 | –5.0 | –5.5 | –4.7 | –5.2 | –4.7 | –5.1 |
| ν∞ [km s-1] | 2790 | 1600 | 1600 | 2400 | 3000 | |||
| νrot [km s-1] | 433 | 335 | 270 | 285 | 253 | |||
| νorbit [km s-1] | 513 | 453 | 423 | 394 | 322 | |||
| X H | 0.75 | 0.17 | 0.1 | 0.05 | 0.0 | |||
| XC [10-3] | 0.15 | 0.01 | 0.01 | 0.01 | 2.12 | |||
| XN [10-3] | 0.04 | 0.54 | 0.54 | 0.54 | 1.22 | |||
| XO [10-3] | 0.4 | 0.01 | 0.01 | 0.01 | 0.06 | |||
|
|
||||||||
| MU [mag] | –6.2 | –6.6 | –6.5 | –6.6 | –5.8 | –5.7 | –5.0 | –4.6 |
| MB [mag] | –5.0 | –5.4 | –5.3 | –5.3 | –4.6 | –4.4 | –3.9 | –3.3 |
| MV [mag] | –4.7 | –5.0 | –5.0 | –5.0 | –4.3 | –4.1 | –3.7 | –3.0 |
| MJ [mag] a | –3.9 | –4.3 | –4.4 | –4.2 | –4.0 | –3.3 | –3.8 | –2.4 |
| MH [mag] a | –3.8 | –4.3 | –4.4 | –4.2 | –4.2 | –3.2 | –4.1 | –2.4 |
| MK [mag] a | –3.6 | –4.3 | –4.5 | –4.0 | –4.5 | –3.1 | –4.5 | –2.5 |
| log QH [s-1] | 49.3 | 49.9 | 50.0 | 50.0 | 50.0 | 50.0 | 49.9 | 49.9 |
| TZanstra,H [kK] | 53.7 | 72.5 | 76.6 | 81.1 | 95.7 | 113.5 | 105.9 | 149.7 |
| log QHe i [s-1] | 48.9 | 49.6 | 49.7 | 49.7 | 49.8 | 49.8 | 49.8 | 49.8 |
| log QHe ii [s-1] | 45.9 | 47.1 | 47.5 | 47.2 | 48.7 | 48.4 | 49.3 | 49.3 |
| TZanstra,He [kK] | 48.0 | 58.9 | 63.4 | 60.8 | 97.4 | 92.5 | 135.9 | 159.3 |
|
|
||||||||
| P [d] | 0.9 | 1.2 | 1.4 | 1.7 | 5.1 | |||
| orbital separation [R⊙] | 18.1 | 21.5 | 23.6 | 26.0 | 32.6 | |||
|
|
||||||||
| Model atom setb | I | II | II | II | III | |||
|
|
||||||||
| Wind accretion rates and accretion X-ray luminosityc | ||||||||
|
|
||||||||
| log Saccr [M⊙/ yr] | –6.9 | –7.4 | –7.4 | –7.9 | –8.0 | –8.4 | ||
| s accr d | 1.3 | 0.4 | 0.4 | 0.1 | 0.1 | 0.04 | ||
| LX [erg s-1]f | 7 × 1038 | 2 × 1038 | 2 × 1038 | 7 × 1037 | 6 × 1037 | 2 × 1037 | ||
Notes. The WN models were calculated with two different mass-loss rates. The “a” models use the same mass-loss rate as given in the tracks, assuming a metallicity scaling of Z0.85 as is observed for O-type stars. The mass-loss rate of the “b” models was scaled according to the mass-loss metallicity relation presented by Hainich et al. (2015).
Model atom set used in the corresponding stellar atmosphere calculations (see Table A.1).
The evolution model predicts BH formation only if the secondary is already in its final evolutionary stage (see text for details). Accretion onto a 36 M⊙ BH is assumed.
Accretion rate normalized to the Eddington accretion rate: 
(see Sect. 5.2 for details).
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