The NewEra model grid | Astronomy & Astrophysics (A&A)

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Fig. 8

Limb darkening for representative giant and dwarf models (as indicated in the panels) for 4 wavelengths. The model with T_eff = 3000 K, log(g) = 0.0 has a mass of 1.35 M_⊙ and the one with T_eff = 3000 K, log(g) = 5.0 has a mass of 0.27 M_⊙. For comparison the simplest plane parallel limb darkening law $I (μ) / I (μ = 1) = \frac{3}{5} (μ + \frac{2}{3})$ $I(\mu) / I(\mu=1)=\frac{3}{5}\left(\mu+\frac{2}{3}\right)$ is shown as a dotted curve.

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