Upper panel: mean magnetic field strength computed from the BOREAS subroutine as a function of stellar angular velocity normalized to the Sun’s velocity. The Sun’s range of B_∗f_∗ = 2 − 7.7  G is shown as a vertical bar. The upper and lower dotted lines illustrate B_∗f_max and B_∗f_min, respectively. The red dashed line is a power-law fit to B_∗f_∗ in the non-saturated regime (cf. Eq. (12)). Middle panel: the mass-loss rate computed from the BOREAS subroutine as a function of stellar angular velocity normalized to the Sun’s velocity. The range of Ṁ estimate for the Sun is shown with a vertical bar. The red dashed line is a power-law fit to Ṁ in the non-saturated regime (cf. Eq. (14)). Lower panel: the angular momentum loss rate as a function of angular velocity. Both quantities are normalized to the Sun’s (, and Ω_⊙ = 2.87 × 10^-6  s^-1). Three overlapping curves are illustrated for fast (blue), median (green), and slow (red) rotator models. The temporal evolution of T_eff and R_∗ is included in the computation of for each model.