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Space-based asteroseismology has opened a window into the interiors of red giants. Mixed modes \cite{Beck_2011} have made it possible to distinguish between hydrogen and helium-burning red giants \cite{Bedding_2011,Mosser_2014}. The rotational splitting of mixed modes has been used to determine the degree of radial differential rotation in red giants, revealing that the cores of red giant stars rotate faster than their envelopes \cite{Beck_2012,Mosser_2012}.  The amplitudes of the stellar oscillations depend on the interplay between driving and damping of the modes \cite{Dupret_2009}. {\bf Interestingly, a group of red giants with suppressed dipole modes were identified using {\it Kepler} observations{\bf  (\cite{Mosser_2011}, see also Figure \ref{fig:moneyplot}).} These stars have normal radial pulsation modes (spherical harmonic degree $\ell=0$), but exhibit low-amplitude dipole ($\ell=1$) modes. Until now, the suppression mechanism was unknown \cite{Garcia_2014}. Below, we demonstrate that dipole mode suppression results from strong magnetic fields within the cores of these red giants.    
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