deletions | additions       diff --git a/section_Magneto_Gravity_Waves_In__.tex b/section_Magneto_Gravity_Waves_In__.tex  index 3b1c164..33c8a1c 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, the value of both $N$ and $v_A$ will typically  increase from the exterior of the radiative zone inward. Incoming gravity waves become increasingly Alfvenic magneto-gravity waves as they propagate inward  toward the helium core. If the hydrogen burning shell (see Figure \ref{fig:Prop}). For stars with  magnetic field strength becomes strengths  large enough to satisfy equation \ref{eqn:magnetogravity2}, \ref{eqn:vamin},  the waves are very strongly altered by the hit a  magnetic field. They wall where $\omega=\omega_{\rm MG}$. Here, they  may either reflect(i.e., they become evanescent as in equation \ref{eqn:magnetodisp3}),  or they may transform be transmitted  into purely the strongly mangnetized region as  Alfven waves. Both processes are likely to occur for an arbitrary In either case, the effect of the strong magnetic  field geometry. is to prevent the gravity wave ever traveling back toward the surface of the star.  \subsection{Magnetic Greenhouse Effect}