Table 3
Comparison of mass-loss rates obtained with different methods for a hydrogen-free WN star with log L/L⊙ = 5.7 and 20 M⊙.
| Paper | log(Ṁ [M⊙ yr−1]) | |
|---|---|---|
| Z⊙ | 0.5 Z⊙ | |
| Gräfener et al. (2017), s.-analytic(a) | −4.72 | no sol. |
| Gräfener et al. (2017), num.(b) | −4.65 | no sol. |
| Sander & Vink (2020) (D∞ = 50) | −4.61 | −4.75 |
| Sander & Vink (2020) (D∞ = 10) | −4.64 | −4.83(c) |
| this work, T* = 130kK(d) (D∞ = 50) | −4.40 | −4.56 |
| this work, T* = 130kK(d) (D∞ = 10) | −4.42 | −4.83(e) |
| Nugis & Lamers (2000) recipe | −4.52 | −4.66 |
| Hamann95+(f) recipe | −4.40 | −4.65 |
| Yoon (2017) recipe (fWR = 1) | −4.59 | −4.77 |
| Yoon (2017) recipe (fWR = 1.6) | −4.39 | −4.57 |
Notes. The Ṁ determinations by Gräfener et al. (2017) employ the Prad-Pgas-plane with the sonic point conditions using (a) their Eq. (27) and assuming υ∞ = 1800 km s−1 or (b) a numerically integrated dPrad/dr. (c) New calculation, but with T* = 141 kK as in Sander & Vink (2020). (d) Choice of T* based on matched Teff(τcrit) with Grassitelli et al. (2018). (e) Unstable solution close to driving breakdown, see Sect. 3.2. (f) Mass-loss rates from Hamann et al. (1995) divided by a factor 10 and scaled with the Z-dependence from Vink & de Koter (2005), as suggested by Yoon et al. (2006).
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