Table 2.
Predicted X-ray active lifetime (τLx, in millions of years) of each of the 17 BH+O binary models and expected number of wind-fed BH HMXBs (NXRBs, last line), for various combinations of β, η, and γ±.
| (β, η)(a) = (1, 1) | (β, η) = (0.8, 1) | (β, η) = (1, 1/3) | (β, η) = (0.8, 1/3) | |||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| γ± | 1/6 | 1 | 3/2 | 1/6 | 1 | 3/2 | 1/6 | 1 | 3/2 | 1/6 | 1 | 3/2 |
| WR155 | 1.5 | 1.5 | 1.4 | 1.5 | 1.2 | 0.9 | 1.4 | 0.2 | 0.0 | 0.9 | 0.0 | 0.0 |
| WR151 | 3.6 | 1.6 | 1.3 | 2.9 | 1.1 | 0.8 | 1.3 | 0.3 | 0.1 | 0.8 | 0.0 | 0.0 |
| WR139 | 2.0 | 1.0 | 0.8 | 1.6 | 0.6 | 0.5 | 0.8 | 0.2 | 0.1 | 0.5 | 0.0 | 0.0 |
| WR31 | 1.9 | 1.0 | 0.8 | 1.6 | 0.7 | 0.6 | 0.8 | 0.2 | 0.1 | 0.6 | 0.0 | 0.0 |
| WR42 | 1.8 | 0.8 | 0.7 | 1.7 | 0.6 | 0.5 | 0.7 | 0.0 | 0.0 | 0.5 | 0.0 | 0.0 |
| WR47 | 0.6 | 0.4 | 0.4 | 0.6 | 0.4 | 0.3 | 0.4 | 0.1 | 0.0 | 0.3 | 0.0 | 0.0 |
| WR79 | 0.8 | 0.1 | 0.0 | 0.6 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| WR127 | 0.6 | 0.0 | 0.0 | 0.4 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| WR21 | 0.3 | 0.2 | 0.1 | 0.3 | 0.1 | 0.1 | 0.1 | 0.0 | 0.0 | 0.1 | 0.0 | 0.0 |
| WR9 | 0.1 | 0.0 | 0.0 | 0.1 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| WR97 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| WR30 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| WR113 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| WR141 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| WR35a | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| WR11 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| WR133 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 | 0.0 |
| NXRBs(b) | 33.0 | 16.6 | 13.4 | 28.3 | 11.8 | 9.0 | 13.4 | 2.5 | 0.7 | 9.0 | 0.0 | 0.0 |
Notes. The bold highlighted column represents our fiducial case.
NXRBs is the predicted number of wind-fed BH high mass X-ray binaries by considering 0.4 Myr to be the typical lifetime of WR stars. See Sect. 3 for more details.
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