Table 2.
Stellar models with changes in the input physics with respect to model A0.
| Model | Affected | Change in the input physics |
|---|---|---|
| A0 | – | – |
| A1 | Γ1 | EoS: SAHA-S (a), Turbulent mixing: calibrated on helium surface abundance of Kepler F-type stars (b) |
| A2 | μ | Turbulent mixing: homogenising turbulent mixing down to T = 5 × 106 K, and no mixing below |
| A3 | T | Surface penetrative convection: ξPC(c) = 0.2 |
| A4 | T | Surface penetrative convection: ξPC(c) = 1.0 |
| A5 | T | Surface penetrative convection: ξPC(c) = 2.0 |
| A6 | T | Surface penetrative convection: Extension equivalent to model A5 with a smoother transition (β = 0.5) |
| A7 | T | Surface penetrative convection: Extension equivalent to model A5 with a smoother transition (β = 2.0) |
| B1 | T | No atomic diffusion |
| B2 | T | No atomic diffusion, Penetrative convection: ξPC(c) = 2.0 |
| B3 | T | No atomic diffusion, PC: Extension equivalent to model B2 with a smoother transition (β = 0.5) |
| B4 | T | No atomic diffusion, PC: Extension equivalent to model B2 with a smoother transition (β = 2.0) |
Notes.
Verma & Silva Aguirre (2019), we used a turbulent diffusion coefficient because of the strong helium and metal depletions induced by atomic diffusion in F-type stars. This enables us to stay in the parameter space of the equation of state (EoS) for the hydrogen mass fraction (0.10 < X < 0.90).
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