Table 1
Inferred parameters for R 144 from the orbital, light curve, and polarimetric (upper part, Sects. 3.1, 3.5, 3.6) spectral (middle part, Sect. 3.3), and evolutionary (lower part, Sect. 4.1) analyses.
| Parameter | Primary | Secondary | |
|---|---|---|---|
| Spectral type | WN5/6h | WN6/7h | |
| Orbital analysis | |||
| Porb (days) (a) | 74.2074 ± 0.0043 | ||
| T0 (MJD) | 58268.98 ± 0.07 | ||
| e | 0.506 ± 0.004 | ||
| V0 (km s−1) (b) | 210 ± 20 | ||
| ω | 304.6 ± 0.8 | 124.6 ± 0.8 | |
| Ω(c) | 114 ± 9 | ||
| K (km s−1) | 129.5 ± 2.3 | 137.4 ± 2.1 | |
| M sin3 i (M⊙) | 48.3 ± 1.8 | 45.5 ± 1.9 | |
| asin i (R⊙) | 164.0 ± 3.0 | 174.3 ± 2.7 | |
 |
0.94 ± 0.02 | ||
| i (deg) (d) | 60.4 ± 1.5 | ||
| a (R⊙) | 189 ± 5 | 200 ± 4 | |
| Mdyn (M⊙) | 74 ± 4 | 69 ± 4 | |
| Spectral analysis | |||
| f∕ftot(V)(e) | 0.44 (fixed) | 0.56 (fixed) | |
| T* (kK) | 50 ± 2 | 45 ± 2 | |
| T2∕3 (kK) | 45 ± 2 | 40 ± 2 | |
| log Rt (R⊙) | 1.10 ± 0.05 | 1.15 ± 0.05 | |
| log L (L⊙) | 6.44 ± 0.05 | 6.39 ± 0.05 | |
| MV,Smith (mag) | −7.3 ± 0.2 | −7.6 ± 0.2 | |
| EB−V (mag) | 0.20 ± 0.01 | ||
| R* (R⊙) | 22 ± 3 | 26 ± 3 | |
| R2∕3 (R⊙) | 27 ± 3 | 31 ± 3 | |
| D | 10 (fixed) | 10 (fixed) | |
| ξ(R*) | 30 (fixed) | 30 (fixed) | |
| log Ṁ (M⊙ yr−1) | −4.38 ± 0.15 | −4.34 ± 0.15 | |
| v∞ (km s−1) | 1400 ± 100 | 1200 ± 100 | |
| XH | 0.35 ± 0.05 | 0.40 ± 0.05 | |
| XC ∕10−4 | 7 ± 3 | 7 ± 3 | |
| XN ∕10−4 |  |
 |
|
| XO ∕10−4 | ≲0.1 | ≲0.1 | |
| v sin i (km s−1) | ≲80 | ≲100 | |
| veq (km s−1) (f) | ≲100 | ≲120 | |
| Evolution models (g) | |||
| Mev, ini (M⊙) | 148 ± 14 | 132 ± 20 | |
| veq, ini (km s−1) |  |
 |
|
| Mev, cur (M⊙) | 111 ± 12 | 100 ± 12 | |
| veq, cur (km s−1) | ≤20 | ≤10 | |
| Age (Myr) | 1.96 ± 0.21 | 2.10 ± 0.20 | |
Notes. (a) Obtained with the ASAS-SN and TESS data using the pwkit pdm algorithm (Sect. 3.5). (b) The absolute calibration of the systematic velocity is model-dependent and is obtained through calibration with model spectra. The 20 km s−1 uncertainty is a rough estimate. (c) Obtained from polarimetry (Sect. 3.6). (d)Obtained from light-curve analysis (Sect. 3.5). (e)Fixed based on mass-luminosity calibrations for homogeneous stars relying on the derived mass ratio. (f) Assuming the orbital and rotational axes are aligned. (g)Inferred with BONNSAI using tracks calculated by Gräfener (2021).
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