Table 10.
Parameters of some best-fit Clés models of CPD-41° 7742 discussed in Sect. 8.
| Model | Age | Minit | M | R | Teff | k2, un. | k2 | 10−8 Ṁ | αov | 106 DT |
|---|---|---|---|---|---|---|---|---|---|---|
| (Myr) | (M⊙) | (M⊙) | (R⊙) | (K) | (10−3) | (10−3) | (M⊙ yr−1) | (cm2 s−1) | ||
| Model IP | 6.25 | 17.89 | 17.73 | 7.55 | 31 150 | 6.6573 | 6.2738 | 3.67 | 0.20 | 0 |
| IS | 10.11 | 10.11 | 4.26 | 25 292 | 9.7592 | 9.5318 | 4.10 × 10−2 | 0.20 | 0 | |
| Model IIP | 6.13 | 18.07 | 17.91 | 7.57 | 31 300 | 6.7045 | 6.3196 | 3.88 | 0.20 | 0 |
| Model IIS | 7.47 | 9.89 | 9.89 | 4.29 | 24 926 | 9.3022 | 9.0757 | 3.54 × 10−2 | 0.20 | 0 |
| Model IIIP (1) | 6.83 | 17.99 | 17.79 | 7.57 | 31 800 | 6.0474 | 5.6974 | 4.74 | 0.20 | 1.81 |
| Model IIIP (2) | 6.81 | 17.99 | 17.79 | 7.57 | 31 800 | 6.0427 | 5.6930 | 4.73 | 0.25 | 1.41 |
| Model IIIP (3) | 6.80 | 17.99 | 17.79 | 7.57 | 31 800 | 6.0389 | 5.6894 | 4.75 | 0.30 | 1.05 |
| Model IIIP (4) | 6.79 | 17.99 | 17.79 | 7.57 | 31 800 | 6.0358 | 5.6865 | 4.74 | 0.35 | 0.74 |
| Model IIIP (5) | 6.78 | 17.99 | 17.79 | 7.57 | 31 800 | 6.0338 | 5.6846 | 4.75 | 0.40 | 0.48 |
| Model IIIS (1) | 6.99 | 9.96 | 9.95 | 4.27 | 25 045 | 9.4745 | 9.2482 | 3.69 × 10−2 | 0.20 | 0.0 |
| Model IIIS (2) | 7.22 | 9.95 | 9.94 | 4.28 | 25 060 | 9.4014 | 9.1759 | 3.74 × 10−2 | 0.25 | 0.0 |
| Model IIIS (3) | 7.50 | 9.92 | 9.92 | 4.28 | 25 054 | 9.3132 | 9.0888 | 3.74 × 10−2 | 0.30 | 0.0 |
| Model IIIS (4) | 7.72 | 9.92 | 9.92 | 4.29 | 25 075 | 9.2483 | 9.0246 | 3.80 × 10−2 | 0.35 | 0.0 |
| Model IIIS (5) | 7.88 | 9.92 | 9.91 | 4.29 | 25 104 | 9.2097 | 8.9869 | 3.87 × 10−2 | 0.40 | 0.0 |
Notes. Columns (1) and (2) give the name of the model and its current age. Column (3) lists the initial mass of the corresponding evolutionary sequence. Columns (4)–(6) give the mass, radius, and effective temperature. Columns (7) and (8) yield the k2 respectively before and after applying the empirical correction for the effect of rotation of Claret (1999). Column (9) lists the mass-loss rate. Columns (10) and (11) give the overshooting parameter and turbulent diffusion coefficient. Models with subscript P (respectively S) correspond to the models of the primary (respectively secondary) star. Models I and II have DT fixed to 0 cm2 s−1 while Models III let it vary freely.
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