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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