Table 3.
Number of post-MS companions of OB stars in our fiducial synthetic SMC population.
| Total | Case A | Case B | ||||
| OBe | OB | OBe | OB | OBe | OB | |
| He-stars | 223 | 12.1 | 56.5 | 11.1 | 166 | 0.96 |
| – M1,i ≤ 10 M⊙ | 191 | 0.03 | 51.0 | 0 | 140 | 0.03 |
| – M1,i, 10 − 17 M⊙ | 18.4 | 2.52 | 4.86 | 2.52 | 13.6 | 0 |
| – M1,i ≥ 17 M⊙ | 13.6 | 9.53 | 0.61 | 8.60 | 13.0 | 0.93 |
| WR-stars | 3.97 | 2.75 | 0.83 | 2.30 | 3.14 | 0.45 |
| – H-free WR | 0.02 | 0.20 | 0.02 | 0.20 | 0 | 0 |
| – CHE WR | 0 | 0.04 | ||||
| NSs | 92.5 | 6.59 | 7.98 | 6.59 | 84.6 | 0 |
| – bound | 21.0 | 3.74 | 5.41 | 3.74 | 15.6 | 0 |
| – disrupted | 71.5 | 2.85 | 2.57 | 2.85 | 69.0 | 0 |
| BHs | 170 | 40.3 | 5.60 | 22.3 | 165 | 18.0 |
| – CHE BH | 0 | 0.32 | ||||
Notes. Besides the total numbers, we give the numbers emerging from Case A mass transfer, from Case B mass transfer, and from chemically homogeneous evolution (CHE). As OBe stars, we count OB mass gainers that rotate faster than 95% of their critical rotation. For core-helium burning mass donors, we distinguish three different initial mass ranges as indicated, as well as stars with log L/ L⊙ > 5.6 as WR stars.
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