Table 1
Parameters of the stellar atmosphere models calculated for the 60 M⊙ track with Z = 1/10 Z⊙ (Marchant et al. 2016, see track I in Fig. 1).
| Model | MI 1 | MI 2 | MI 3 | MI 4 | MI 5 | |||
| a | b | a | b | a | b | |||
|
|
||||||||
| Spectral type | O3 V((f*))z | O2–3 If* | WN2 | WN2 | WO1 | |||
| age [106 yr] | 0.09 | 3.45 | 4.39 | 4.65 | 4.95 | |||
| T∗ [kK] | 52.2 | 59.4 | 66.0 | 100.0 | 150.0 | |||
| log L [L⊙] | 5.73 | 6.05 | 6.18 | 6.2 | 6.16 | |||
| M [M⊙] | 63.1 | 59.7 | 52.8 | 47.5 | 34.8 | |||
| R∗ [R⊙] | 9.0 | 10.0 | 9.4 | 4.2 | 1.8 | |||
| log Ṁ [M⊙/ yr] | –6.0 | –5.6 | –4.8 | –5.1 | –3.2a | –3.5a | –4.5 | –4.9 |
| ν∞ [km s-1] | 3155 | 1600 | 1600 | 2400 | 3000 | |||
| νrot [km s-1] | 381 | 348 | 221 | 253 | 110 | |||
| νorbit [km s-1] | 493 | 463 | 391 | 342 | 246 | |||
| X H | 0.75 | 0.37 | 0.14 | 0.08 | 0.0 | |||
| XC [10-3] | 0.29 | 0.02 | 0.02 | 0.02 | 450.0 | |||
| XN [10-3] | 0.09 | 1.08 | 1.08 | 0.11 | 0.0 | |||
| XO [10-3] | 0.8 | 0.02 | 0.02 | 0.02 | 147.0 | |||
|
|
||||||||
| MU [mag] | –6.8 | –7.0 | –7.0 | –7.0 | –9.0 | –8.4 | –6.4 | –5.8 |
| MB [mag] | –5.5 | –5.8 | –5.8 | –5.7 | –8.2 | –7.7 | –5.2 | –4.6 |
| MV [mag] | –5.2 | –5.4 | –5.4 | –5.4 | –8.0 | –7.3 | –4.7 | –3.9 |
| MJ [mag] b | –4.4 | –4.6 | –4.9 | –4.7 | –8.1 | –7.4 | –4.7 | –3.7 |
| MH [mag] b | –4.3 | –4.6 | –4.9 | –4.7 | –8.4 | –7.7 | –5.0 | –4.0 |
| MK [mag] b | –4.0 | –4.4 | –5.1 | –4.6 | –8.7 | –8.3 | –5.3 | –4.3 |
| log QH [s-1] | 49.5 | 49.9 | 50.1 | 50.1 | 49.8 | 51.2 | 49.9 | 49.9 |
| TZanstra,H [kK] | 52.0 | 65.9 | 68.8 | 72.7 | 30.6 | 77.7 | 81.5 | 109.3 |
| log QHe i [s-1] | 49.1 | 49.5 | 49.7 | 49.7 | 49.3 | 51.2 | 49.8 | 49.8 |
| log QHe ii [s-1] | 45.1 | 46.5 | 41.9 | 46.0 | 37.4c | 41.5c | 48.9 | 49.1 |
| TZanstra,He ii [kK] | 40.6 | 50.8 | 26.8 | 46.0 | 17.4c | 23.7c | 98.8 | 125.0 |
|
|
||||||||
| P [d] | 1.2 | 1.4 | 2.1 | 2.9 | 5.6 | |||
| orbital separation [R⊙] | 23.8 | 26.5 | 33.0 | 38.6 | 54.7 | |||
|
|
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| Model atom setd | I | I | I | II | III | |||
|
|
||||||||
| Wind accretion rates and accretion X-ray luminositye | ||||||||
|
|
||||||||
| log Saccr [M⊙/ yr] | –7.0 | –7.3 | –6.2 | –6.5 | –8.2 | –8.6 | ||
| s accr f | 1.1 | 0.5 | 6.3 | 3.1 | 0.06 | 0.03 | ||
| LX [erg s-1]g | 6 × 1038 | 3 × 1038 | 3 × 1039 | 2 × 1039 | 4 × 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 it is observed for O-type stars. The mass-loss rates of the “b” models were scaled according to the mass-loss metallicity relation presented by Hainich et al. (2015).
The high mass-loss rate of this model is a result of the high angular velocity, leading to a rotational enhancement of Ṁ compared to a non-rotating model. For details, we refer the reader to Marchant et al. (2016).
Only lower limits, since the He ii ionization edge is optically thick at the outer boundary of the respective stellar atmosphere models.
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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