Table 1
Input parameters, clumping stratification, and predicted wind properties of our best-fit R144-primary, R144-secondary, and R136al hydro-dynamic models.
| Parameter | R144-prim | R144-sec | R136a1 Fixed Dcl | R136a1 Fixed M, vturb tests | ||
|---|---|---|---|---|---|---|
| spectral type | WN5/6h | WN6/7h | WN5h | WN5h | WN5h | WN5h |
| T⋆[kK] | 49.3 | 45.5 | 46.8 | 46.8 | 47.5 | 48 |
| Teff(τRoss = 2/3) [kK] | 45.6 | 41.4 | 46 | 46.2 | 46.1 | 45.7 |
| log(L⋆/L⊙) | 6.44 | 6.39 | 6.79 | 6.79 | 6.79 | 6.79 |
| R⋆/R⊙ | 22.81 | 25.28 | 37.87 | 37.87 | 36.76 | 36 |
| RτRoss = 2/3/R⊙ | 26.62 | 30.41 | 38.78 | 38.82 | 39.01 | 39.74 |
| M⋆/M⊙ | 74 | 70 | 233 | 242.1 | 242.1 | 242.1 |
| X | 0.25 | 0.3 | 0.5 | 0.5 | 0.5 | 0.5 |
| vturb [km s−1] | 21.21 | 21.21 | 21.21 | 21.21 | 70.71 | 100 |
| Dcl,∞ | 30 | 22 | 45 | 45 | 40 | 42 |
| vcl [km s−1] | 90 | 125 | 100 | 23 | 75 | 82 |
log(![$\[\dot{M}\]$](/articles/aa/full_html/2025/04/aa53447-24/aa53447-24-eq26.png) ) |
−4.572 | −4.649 | −4.686 | −4.692 | −4.747 | −4.74 |
| v∞[km s−1] | 1361.4 | 1257.9 | 2649.03 | 2722.8 | 2699 | 2672.4 |
log(![$\[\dot{M}\]$](/articles/aa/full_html/2025/04/aa53447-24/aa53447-24-eq27.png) t) |
−4.297 | −4.370 | −4.875 | −4.893 | −4.970 | −4.947 |
| v(r = rsonic) [km s−1] | 20.53 | 19.53 | 19.99 | 21.07 | 19.1 | 20.98 |
| v(r = rcrit) [km s−1] | 29.27 | 28.46 | 29.06 | 29.82 | 73.14 | 101.73 |
| βeff,in | 2.6 | 2 | 2.4 | 2.3 | 2.9 | 3.3 |
| βeff,out | 1.3 | 1.3 | 0.9 | 0.9 | 1 | 1 |
| Γe,R⋆ | 0.713 | 0.701 | 0.608 | 0.574 | 0.591 | 0.588 |
| τF,sonic | 1.779 | 1.596 | 0.767 | 0.693 | 0.778 | 0.859 |
| τF,crit | 1.592 | 1.383 | 0.734 | 0.666 | 0.576 | 0.541 |
| log(QH I[ phot s−1]) | 50.30 | 50.25 | 50.66 | 50.65 | 50.66 | 50.67 |
| log(QHe I[ phot s−1]) | 49.73 | 49.62 | 50.10 | 50.07 | 50.12 | 50.14 |
| log(QHe II[ phot s−1]) | 40.17 | 40.05 | 41.17 | 41.23 | 41.20 | 41.24 |
Notes. The inputs we adopt from previous literature are marked in bold-faced text. For R144-primary and secondary components, we adopt the luminosities and the dynamical masses from Shenar et al. (2021). The surface H for R144 were also initially adopted from Shenar et al. (2021), but was later reduced by 0.1 to achieve better fits to H/He lines. For R136a1, the luminosities and surface H are adopted from Bestenlehner et al. (2020), and the masses are from homogeneous relations from Gräfener et al. (2011).
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