Table 3
Lifetime of the spectroscopic phases of a non-rotating 60 M⊙ star.
| Spectral type | Previous duration | Revised duration |
| (chem. abund., yr ) | (spec. class., yr) | |
|
|
||
| O | 3.00 × 106 | 3.22 × 106 |
| BHG | − | 0.79 × 105 |
| LBV | − | 2.35 × 105 |
| WR | 3.97 × 105 | 3.95 × 105 |
| WNL | 6.13 × 104 | 0.49 × 104 |
| WNE | 5.15 × 104 | 10.31 × 104 |
| WC | 2.85 × 105 | 2.57 × 105 |
| WO | − | 3.77 × 104 |
|
|
||
| τLBV,60,0/τO,60,0 = 0.073 | ||
| τWR,60,0/τO,60,0 = 0.120 | ||
| τLBV,60,0/τWR,60,0 = 0.594 | ||
Notes. Column 2 refers to the previous values found using chemical abundance and Teff criteria (from Georgy et al. 2012), while Col. 3 shows the revised durations obtained in this work through a classification of the synthetic spectra from the evolutionary models. The timescales of the LBV (τLBV,60,0), WR (τWR,60,0), and O-type phases (τO,60,0) for a non-rotating 60 M⊙ star are indicated at the bottom of the table.
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