Table 3
Rotational properties inferred from photometric variability.
| WR | P | τ hyd | νesc | νcrit | νrot | log (j) |
|
Ref. |
| [d] | [d] | [ ] |
[] |
[] |
[ ] |
[105 yr] | ||
|
|
||||||||
| 006 | 3.77 | 0.02 | 1605 | 920 | 36 | 17.8 | 1.8 | (1) |
| 016 | 10.7 | 0.18 | 787 | 411 | 58 | 18.7 | 4.0 | (2) |
| 040 | 4.76 | 0.15 | 809 | 444 | 113 | 18.9 | 1.8 | (2) |
| 134 | 2.25 | 0.05 | 1136 | 651 | 119 | 18.6 | 2.3 | (3) |
| 136 | 4.55 | 0.03 | 1250 | 731 | 37 | 17.9 | 2.2 | (4) |
| 137 | 0.83 | 0.03 | 1266 | 743 | 226 | 18.7 | 2.0 | (5) |
Notes. The given values are based on the stellar parameters from Table 2, and observed photometric periods P. Given are hydrostatic adjustment timescales 
, escape velocities νesc = (2GM⋆/R⋆)1/2, critical rotation velocities νcrit = (GM⋆(1 − Γe)/R⋆)1/2, rotational velocities νrot = 2πR⋆/p, and specific angular momenta j = R⋆νrot. Mass-loss timescales M⋆/Ṁ are given dependent on the wind clumping factor D (cf. Table 2). References for the photometric periods are (1) Morel et al. (1997); (2) Lamontagne & Moffat (1987); (3) Morel et al. (1999); (4) St.-Louis et al. (1989); (5) Lefèvre et al. (2005).
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