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The amplitudes of these oscillations depend on the interplay between driving and damping of the modes \citep{Dupret_2009}. Interestingly, a significant group of red giants with suppressed dipole modes were identified using {\it Kepler} observations (e.g., \citealt{Mosser_2011}, see Figure \ref{fig:moneyplot}). These stars have normal radial pulsation modes (spherical harmonic degree $\ell=0$), but exhibit low-amplitude dipolar ($\ell=1$) modes.  %They comprise about $20 \%$ of stars on the early red giant branch (RGB) in the sample presented in \citet{Mosser_2011}.   Until now, the suppression mechanism was unknown \citep{Garcia_2014}. Below, we demonstrate that dipole mode suppression results from strong magnetic fields within the cores of these  red giants. %Here, we demonstrate that the presence of a strongly magnetized core suppresses the visibility of dipolar modes via a ``magnetic greenhouse" effect. We show that magnetic suppression reduces the visibility of dipole modes to the level observed by \citet{Mosser_2011} in suppressed dipolar pulsators, suggesting these stars host strong magnetic fields in their cores. We develop a novel asteroseismic technique that places tight constraints on (and in some cases yields measurements of) the magnetic fields in red giant cores.