Table B.1
Summary of important stellar characteristics.
M i | v rot,i | τ MS | log Li/L⊙ | T eff,i | M conv,i | M over,i | M conv,0.2 | M over,0.2 | M f | v rot,f | Y s,f | Y c,f | log Lf/L⊙ | T eff,f | j | |
M ⊙ | km s-1 | Myr | K | M ⊙ | M ⊙ | M ⊙ | M ⊙ | M ⊙ | km s-1 | K | 1015 cm2/s | |||||
|
||||||||||||||||
60 | 0 | 3.373 | 5.704 | 50 000 | 42.6 | – | 30.7 | – | 43 | 0 | 0.393 | 0.995 | 6.022 | 6600 | 0 | |
60 | 220 | 3.407 | 5.701 | 49 500 | 43.8 | – | 30.7 | – | 42 | 0 | 0.398 | 0.995 | 6.023 | 8800 | 89 | |
60 | 273 | 3.464 | 5.699 | 49 200 | 43.6 | – | 30.8 | – | 42 | 0 | 0.384 | 0.995 | 6.023 | 5600 | 89 | |
60 | 326 | 3.619 | 5.698 | 48 900 | 43.5 | 3.0 | 32.4 | 2.6 | 45 | 1 | 0.418 | 0.995 | 6.056 | 14 200 | 85 | |
60 | 379 | 3.676 | 5.694 | 48 600 | 43.4 | 3.1 | 32.7 | 2.6 | 45 | 1 | 0.412 | 0.995 | 6.061 | 14 800 | 84 | |
60 | 432 | 4.038 | 5.691 | 48 300 | 43.3 | 3.1 | 38.6 | 2.1 | 45 | 518 | 0.677 | 0.995 | 6.133 | 38 900 | 237 | |
60 | 532 | 4.167 | 5.684 | 47 600 | 43.0 | 3.2 | 40.4 | 1.6 | 38 | 383 | 0.865 | 0.995 | 6.098 | 69 600 | 212 | |
100 | 0 | 2.648 | 6.102 | 54 100 | 80.6 | 3.8 | 57.2 | 3.8 | 68 | 0 | 0.636 | 0.993 | 6.336 | 17 600 | 0 | |
100 | 217 | 2.692 | 6.099 | 53 700 | 82.1 | 3.6 | 57.4 | 3.7 | 66 | 1 | 0.674 | 0.991 | 6.331 | 22 200 | 98 | |
100 | 271 | 2.740 | 6.098 | 53 500 | 81.9 | 3.5 | 58.2 | 3.7 | 65 | 12 | 0.722 | 0.993 | 6.337 | 27 800 | 97 | |
100 | 323 | 2.817 | 6.096 | 53 200 | 81.7 | 4.3 | 60.1 | 3.5 | 67 | 7 | 0.720 | 0.993 | 6.354 | 26 400 | 105 | |
100 | 375 | 2.973 | 6.094 | 53 000 | 81.6 | 3.5 | 66.3 | 2.6 | 61 | 64 | 0.929 | 0.991 | 6.345 | 47 700 | 130 | |
100 | 426 | 3.016 | 6.093 | 52 700 | 81.4 | 3.5 | 66.3 | 2.2 | 50 | 39 | 0.974 | 0.993 | 6.236 | 58 900 | 88 | |
100 | 524 | 3.065 | 6.088 | 52 100 | 81.0 | 3.7 | 66.1 | 1.8 | 46 | 64 | 0.975 | 0.995 | 6.213 | 73 000 | 83 | |
150 | 0 | 2.313 | 6.382 | 56 000 | 131.6 | 3.7 | 91.3 | 4.4 | 94 | 0 | 0.839 | 0.975 | 6.553 | 30 200 | 0 | |
150 | 216 | 2.339 | 6.381 | 55 600 | 131.3 | 4.1 | 91.5 | 4.4 | 94 | 4 | 0.836 | 0.973 | 6.553 | 30 200 | 121 | |
150 | 268 | 2.417 | 6.380 | 55 400 | 131.1 | 3.7 | 95.4 | 4.2 | 99 | 11 | 0.821 | 0.966 | 6.573 | 28 900 | 144 | |
150 | 320 | 2.465 | 6.378 | 55 200 | 130.9 | 3.8 | 97.9 | 3.5 | 91 | 17 | 0.931 | 0.966 | 6.550 | 41 100 | 139 | |
150 | 371 | 2.544 | 6.377 | 55 000 | 130.7 | 3.9 | 98.0 | 2.3 | 57 | 15 | 0.978 | 0.991 | 6.313 | 55 000 | 47 | |
150 | 421 | 2.557 | 6.376 | 54 700 | 130.6 | 3.8 | 96.8 | 2.1 | 55 | 17 | 0.979 | 0.993 | 6.300 | 56 400 | 48 | |
150 | 514 | 2.579 | 6.372 | 54 200 | 130.2 | 3.9 | 95.3 | 2.1 | 55 | 17 | 0.977 | 0.991 | 6.293 | 55 600 | 51 | |
200 | 0 | 2.140 | 6.567 | 56 200 | 181.5 | 3.9 | 126.1 | 4.7 | 131 | 0 | 0.809 | 0.916 | 6.698 | 30 700 | 0 | |
200 | 214 | 2.155 | 6.566 | 55 800 | 181.1 | 4.0 | 125.4 | 4.7 | 126 | 9 | 0.843 | 0.927 | 6.693 | 32 300 | 159 | |
200 | 267 | 2.185 | 6.565 | 55 600 | 180.9 | 3.9 | 126.7 | 5.6 | 133 | 8 | 0.792 | 0.912 | 6.700 | 30 300 | 190 | |
200 | 318 | 2.255 | 6.564 | 55 400 | 180.7 | 4.0 | 130.2 | 3.8 | 70 | 2 | 0.986 | 0.995 | 6.436 | 51 100 | 37 | |
200 | 367 | 2.291 | 6.563 | 55 300 | 180.6 | 3.9 | 129.1 | 2.8 | 64 | 3 | 0.985 | 0.995 | 6.383 | 53 800 | 37 | |
200 | 415 | 2.302 | 6.562 | 55 100 | 180.4 | 4.1 | 127.6 | 2.3 | 65 | 2 | 0.980 | 0.991 | 6.387 | 50 900 | 41 | |
200 | 502 | 2.334 | 6.560 | 54 700 | 179.8 | 4.1 | 121.7 | 2.1 | 62 | 6 | 0.979 | 0.991 | 6.362 | 52 400 | 43 | |
300 | 0 | 1.979 | 6.811 | 54 500 | 281.1 | 4.7 | 195.3 | 4.7 | 82 | 0 | 0.988 | 0.993 | 6.519 | 46 800 | 0 | |
300 | 213 | 2.003 | 6.810 | 54 300 | 280.6 | 3.8 | 193.4 | 4.9 | 80 | 1 | 0.988 | 0.993 | 6.509 | 47 300 | 17 |
Notes. From left to right: mass and surface rotational velocity at the ZAMS (index i); main-sequence lifetime; luminosity and effective temperature at the ZAMS; mass of the convective core and the overshoot zone at the first calculated model after the ZAMS and when hydrogen in the core drops below 0.2; mass, surface rotational velocity, helium mass fraction at the surface and in the core, luminosity, effective temperature; and surface specific angular momentum at the end of the main sequence evolution (index f). Several stellar evolution models have not been calculated until the TAMS. In these cases, the main sequence lifetime is extrapolated until the exhaustion of hydrogen in the core and the final values in Cols. 6–16 correspond to the last calculated values. Dashes in the table indicate data which is not available.
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