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Surface magnetic fields are routinely measured in stars. However internal magnetic fields are inaccessible to direct observations and very little is known about their amplitude, geometry and evolution.  %A fraction of main-sequence A stars shows strong surface magnetic fields (Ap stars).  %Ap stars have large scale, predominantly dipolar magnetic fields that show little or no time evolution and %amplitudes in the range 0.3-30kG.   In this paper we demonstrate that a strong magnetic field in the core of red giant stars can suppress the amplitude of dipolar oscillation modes. Suppressed dipolar modes are indeed observed in a fraction of ascending RGB stars, and we identify interpret  these as stars with strongly magnetized cores. We are able to put strong constraints place lower limits  on theamplitude of the  internal magnetic fields field strength  in stars with suppressed dipolar modes. The inferred values, together with the observed fraction, suggests that some of magnetic fields indicate  these stars could be are  the descendants of magnetic Ap stars. stars, or hosted a powerful core dynamo during the main sequence.  The novel asteroseismic technique reported here allowsto constrain  for the first time the constraints on  magnetic field fields  in the deep interiors of a large population of stars.