Table 1.
Models used for comparison.
| Name | Code | Base model | L⋆ (L⊙) | Teff (K) | Notes |
|---|---|---|---|---|---|
| CO5BOLD mean | CO5BOLD | st28gm06n26 | 6955 | 2737 | Mean structure of a 3D model. |
| CO5BOLD x-dir | CO5BOLD | st28gm06n26 | 6955 | 2737 | Local structure of a 3D model. |
| DARWIN u2 | DARWIN | l70t27 | 7000 | 2700 | Δup = 2 (from Eqs. (1) and (2)) |
| DARWIN u4 | DARWIN | l70t27 | 7000 | 2700 | Δup = 4 (from Eqs. (1) and (2)) |
Notes. Two ways are used to extract radial velocities and luminosity from a 3D model, either by considering the mean behaviour of the structure or the local behaviour (see Sect. 3 for more detailed explanation). This is compared to two DARWIN models, with the same stellar parameters but different inner boundary conditions.
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