Table 1
Main ingredients of the evolutionary models.
| STERN1 | Geneva2 | FRANEC3 | Padova4 | MESA5 | STAREVOL5 | |
|
|
||||||
| Initial metallicity (Z) | 0.0088 | 0.0140 | 0.01345 | 0.0170 | 0.014 | 0.0134 |
| Mixing length parameter (l/HP) | 1.5 | 1.6 / 1.0† | 2.3 | 1.68 | 2.0 | 1.63 |
| Overshoot parameter (d/HP) | 0.335 | 0.1 | 0.2 | ~0.5 | f = 0.0/0.01/0.02‡ | 0.0/0.1/0.2 |
| Rotation | 0−550 km s-1 | Ω/Ωcrit = 0.4 | 300 km s-1 | 0 | 0/200 km s-1 | 0/220 km s-1 |
| Magnetic field | Spruit-Taylor | no | no | no | no | no |
| Solar mixture | AGS056 | AGS05 | AGSS097 | GN938 | GN93 | AGSS09 |
| with C, N, O, | with Ne enhanced | |||||
| Mg, Si, Fe modified | (Cunha et al. 2006) | |||||
Reference. 1) Brott et al. (2011a); 2) Ekström et al. (2012); 3) Chieffi & Limongi (2013); 4) Bertelli et al. (2009); 5) this work. Heavy elements solar mixture: 6) Asplund et al. (2005); 7) Asplund et al. (2009); 8) Grevesse et al. (1993). †For stars with initial mass <40 M⊙, the mixing length parameter is l/HP = 1.6. For more massive stars, it is defined with respect to the local density scale height and l/Hρ = 1.0. ‡In MESA the overshooting is implemented as a decreasing exponential with parameter f (see text).
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