Considered magnetic field configurations at different evolutionary stages of a typical 1.5 M_⊙ star. The central field strengths are set such that asteroseismic detections of all three fields would measure 100 kG during the RGB stage (see Appendix C). Left panel: Scenarios A (dark blue line) and B (light blue line) are created by the convective core during the MS stage and start evolving as a large-scale stable field at the end of the MS. Middle panel: Magnetic fields during the RGB stage when the typical oscillation frequency of the star reaches 150 μHz. The two fields for Scenarios A and B are now buried below the hydrogen-burning shell (dashed line). Scenario C (red line) starts its evolution here and fills the entire radiative interior. Right panel: Magnetic field configurations for all three scenarios at the start of the WD cooling sequence. The blue-shaded region corresponds to the radial extent of the WD mass at different evolutionary stages.