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Table 4.
Relative abundances of the different phases in populations of massive stars between 20 M⊙ and 120 M⊙, assuming constant star formation rate, a power-law IMF from Salpeter (1955), and different MS mass-loss rates and different metallicities.
| Relative abundance [%] | ||||
|---|---|---|---|---|
| Phase | Z = 0.014 | Z = 0.006 | ||
| Vin01 | Bes20 | Vin01 | Bes20 | |
| MS | 89.9 | 89.8 | 90.1 | 90.2 |
| RSG | 3.2 | 3.0 | 1.0 | 0.9 |
| YSG | 1.8 | 3.5 | 2.0 | 2.1 |
| BSG | 3.5 | 2.4 | 6.1 | 6.4 |
| WR | 1.6 | 1.3 | 0.8 | 0.4 |
| WNH | 0.3 | 0.5 | 0.4 | 0.3 |
| WN | 0.2 | 0.2 | 0.1 | 0.1 |
| WC | 1.1 | 0.6 | 0.3 | 0.1 |
| WO | < 0.05 | |||
Notes. The values are numerical results rounded to one decimal place.
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