deletions | additions       diff --git a/section_Magneto_Gravity_Waves_In__.tex b/section_Magneto_Gravity_Waves_In__.tex  index 335d739..0f994e0 100644  --- a/section_Magneto_Gravity_Waves_In__.tex  +++ b/section_Magneto_Gravity_Waves_In__.tex 
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\omega_{MG} = \sqrt{2 v_A N k_\perp} \, .  \end{equation}  In a magnetized red giant core, both $N$ and $v_A$ will typically increase from the exterior of the radiative zone inward toward the hydrogen burning shell. Figure \ref{Fig:cartoon} \ref{fig:cartoon}  illustrates the general properties of waves that produce solar-like oscillations in red giants. In stars with large enough field strengths to satisfy equation \ref{eqn:vamin} somewhere in their core, incoming gravity waves will become evanescent where $\omega=\omega_{\rm MG}$ see Figure \ref{fig:Prop}). At this point, the waves must either reflect or be transmitted into the strongly magnetized region as Alfven waves. In both cases, the waves will be prevented from returning to the surface of the star to be observed as solar-like oscillations.