deletions | additions       diff --git a/Introduction.tex b/Introduction.tex  index f7ec840..4863f7f 100644  --- a/Introduction.tex  +++ b/Introduction.tex 
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%For example, it is not clear if some of the magnetic flux observed at the surface of main sequence stars can be conserved through the various phases of stellar evolution and be responsible for the existence of strongly magnetized compact remnants such as magnetic white dwarfs and neutron stars \cite{Wickramasinghe_2000,Duncan_1992}. Magnetic fields at stellar surfaces are routinely observed through their Zeeman spectral signature \cite{Landstreet_1992}. About 5-10\% of main sequence A stars are observed to have large scale, predominantly dipolar magnetic fields with surface strengths $0.3$-$30\, {\rm kG}$ (Ap stars, see e.g. \cite{Auri_re_2007}). Surface magnetic fields have also been detected in a handful of evolved red giant stars \cite{Auri_re_2015}. In Ap stars, the fields show little or no time evolution, which together with the existence of stable magnetic configurations \cite{Braithwaite_2004,Duez_2010} supports the notion that they are not generated by a contemporary magnetic dynamo but rather inherited from the star formation phase (i.e., a fossil field).   After exhausting hydrogen in their cores, most main sequence stars evolve up the red giant branch (RGB). During this phase, the stellar structure is characterized by an expanding convective envelope and a contracting radiative core. Acoustic waves (p modes) in the envelope can couple to gravity waves (g modes) in the core {\bf \cite{Bedding_2014}}. Consequently, non-radial stellar oscillation modes become mixed modes that probe both the envelope (the p mode cavity) and the core (the g mode cavity), {\bf as illustrated in Figure \ref{fig:cartoon}.} 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}, {\bf and to measure the rotation rate of red giant cores (\cite{Beck_2012,Mosser_2012}.} (\cite{Beck_2012,Mosser_2012}.)}  The amplitudes of the stellar oscillations depend on the interplay between driving and damping of the modes {\bf \cite{Dupret_2009,Benomar_2014}.} {\bf A group of red giants with depressed dipole modes were identified using {\it Kepler} observations (\cite{Mosser_2011}, see also Figure \ref{fig:moneyplot}).} {\bf These stars show normal radial modes} (spherical harmonic degree $\ell=0$), {\bf but exhibit dipole ($\ell=1$) modes whose amplitude is much lower than usual.} Until now, the depression mechanism was unknown \cite{Garcia_2014}. Below, we demonstrate that dipole mode depression {\bf may result} from strong magnetic fields within the cores of these red giants. 
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