deletions | additions       diff --git a/Introduction.tex b/Introduction.tex  index 9dc8493..8241dd4 100644  --- a/Introduction.tex  +++ b/Introduction.tex 
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%In this situation some of the energy in the p-modes can leak into the g-modes cavity, where waves with frequency $\omega < N$ can be excited ($N$ is the Brunt-Vaisala frequency).  Space-based asteroseismology has opened a window into the interiors of red giants. Mixed modes \citep{Beck_2011} have made it possible to distinguish between hydrogen and helium-burning red giants \citep{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 much faster than their envelopes \citep{Beck_2012}. \cite{Beck_2012}.  %but much slower than predicted by theory \citep{Cantiello_2014}.   The amplitudes of solar-like oscillations depends on the interplay between driving and damping of the modes \citep{Dupret_2009}. Interestingly, a group of red giants with very weak dipole modes has been identified by \citet{Mosser_2011} (see Figure \ref{fig:moneyplot}). These stars have normal radial pulsation modes (spherical harmonic degree $\ell=0$) , but exhibit suppressed dipolar ($\ell=1$) modes. They comprise about $20 \%$ of stars on the lower red giant branch (RGB) in the sample presented in \citet{Mosser_2011}. Until now, the suppression mechanism was unknown. Below, we demonstrate that dipole mode suppression results from strong magnetic fields within the cores of red giants.