Hertzsprung–Russell diagram of our models. The data points correspond to the γ Dor stars studied in this work from Li et al. (2020); the points are semi-transparent to illustrate the number density when two or more stars overlap. The typical uncertainty on effective temperature and luminosity is shown in the figure. The stellar models are computed from the ZAMS with an initial metallicity of Z = 0.01 and an initial rotation rate Ω/2π = 20 μHz (no magnetic fields); initial masses are indicated in solar masses for each track.