Considering again the low-mass stars (\(< 1.1\)\(\mathrm{M}_\odot\)), of which none show suppression, we see from Figure 4 that radial magnetic fields above \(\approx 100 \, {\rm kG}\) are not present at the hydrogen-burning shell when the stars are just below the red giant luminosity bump (\(\nu_\mathrm{max}\) \(\approx 70-100 \, \mu{\rm Hz}\)). Assuming magnetic flux conservation from the main-sequence phase, this suggests that radial fields above \(\approx 5 \, {\rm kG}\) do not exist within the cores of Sun-like stars \citep{Fuller15}. Large scale fields in the solar interiors have been discussed in order to explain the properties of the tachocline \citep{GoughMcIntyre98}. However, our results do not rule out strong horizontal fields near the radiative-convective boundary because those fields would be outside the core and could not cause mode suppression when the star evolves into a red giant.