Trapped fraction evaluated with Eq. (13) at ω = 2πν_max, where ν_max is the frequency of maximum oscillation power, as a function of the evolution of the star indicated by ν_max (stars evolve from right to left). Each panel features one of the four evolutionary tracks presented in Fig. 1. Rows show tracks with the same stellar mass and columns show tracks with the same metallicity. The blue (red) lines correspond to the dipole (quadrupole) modes. Different linestyles (solid, dashed, dotted) represent different initial strengths of the radial component of the magnetic field at the stellar center, which corresponds to the field strength the end of the MS. Due to the conservation of magnetic flux, the magnetic field strength increases as the stars evolve. The small knees that occur at the points where f_T becomes greater than 0, which are visible in some of the curves, are caused by the limited temporal resolution of the evolutionary tracks. We show the evolution of the trapped fraction considering B_H/B_crit, H instead of B_cen/B_crit, cen in Fig. B.4.