deletions | additions       diff --git a/Abstract.tex b/Abstract.tex  index 6b58af5..c656d41 100644  --- a/Abstract.tex  +++ b/Abstract.tex 
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%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.  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 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 significant  fraction of ascending RGB stars, and we stars. We  interpret these as stars with strongly magnetized cores. We cores, and we  place lower limits on the internal magnetic field strength in stars with suppressed dipolar modes. The inferred magnetic fields indicate these stars are the descendants of magnetic Ap stars, or hosted a powerful core dynamo during the main sequence. The novel asteroseismic technique reported here allows for constraints on magnetic fields in the deep interiors of a large population of stars.