deletions | additions       diff --git a/Introduction.tex b/Introduction.tex  index 6589e43..d9eaae0 100644  --- a/Introduction.tex  +++ b/Introduction.tex 
...
% Acoustic waves excited by turbulent convection in the envelope can propagate through the star and be used to %probe the stellar interiors. Asteroseismology of thousands of red giants has just become possible thanks to the %space satellites CoRoT and Kepler. During the red giant branch (RGB) the frequency of stochastically generated %acoustic waves (p-modes) becomes comparable to the frequency of internal gravity waves (g-modes) in the radiative %core of the star. In this situation a crosstalk between p-modes and g-modes becomes possible if enough energy can %leak through the evanescent region, which is located between the acoustic cavity and the gravity-waves cavity and %which extent depends on the harmonic degree ($\ell$) of the mode.  %This gives rise to standing waves with a mixed nature (mixed modes). The restoring force for these waves is the %pressure gradient in the envelope and gravity in the core.   %The rotational splitting of mixed modes has been used to determine the degree of differential rotation in red %giants interiors, revealing that the core of these stars is rotating about 10 times faster than their envelope %\cite{Beck_2011}.  Acoustic waves (p-modes) excited by turbulent convection in red giant envelopes can couple to internal gravity waves. This is because, as a red giant increase its radius, the frequency $\omega$ of p-modes decreases and becomes comparable to the frequency of waves in the g-mode cavity. 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). These pulsation modes, called mixed-modes, are characterized by significant displacements in both the envelope and the core of a red giant. In the era of space asteroseismology this offers a new window to probe the internal properties of stars. For example  the rotational splitting of mixed modes has beenobserved by the Kepler satellite; this data has been  used to determine the degree of differential rotation in red giants interiors, revealing that the core of red giant stars is rotating about 10 times faster than their envelope \cite{Beck_2011}.The amplitude and observability of stochastically excited pulsations in red giant branch (RGB) stars depends on the interplay between driving and damping of the modes \citet{Dupret_2009}. A family of red giants with very weak dipole modes has been identified by \citet{Mosser_2011}. These stars have normal radial ($\ell=1$) pulsation modes, but exhibit depressed dipolar $\ell=1$ modes.  Magnetic The amplitude and observability of stochastically excited pulsations in red giant branch (RGB) stars depends on the interplay between driving and damping of the modes \citet{Dupret_2009}. Interestingly a family of red giants with very weak dipole modes has been identified by \citet{Mosser_2011}. These stars have normal radial ($\ell=0$) pulsation modes, but exhibit depressed dipolar ($\ell=1$) modes. Here we demonstrate that the presence of a strongly magnetized core affects the visibility of dipolar modes at the level observed in the data. We develop a novel asteroseismic technique allowing to detect the presence and the amplitude of magnetic  fieldsunobserved  in the deep stellar  interiors. Red giant asteroseismology. Depressed dipoles mistery. We demonstrate that the presence of a strongly magnetized core affects the visibility of dipolar modes at the level observed in the data, suggesting that the suppressed dipole stars in \citet{Mosser_2011} host strong magnetic fields in their cores.  \begin{itemize}