deletions | additions       diff --git a/section_Magneto_Gravity_Waves_In__.tex b/section_Magneto_Gravity_Waves_In__.tex  index 8ae0473..2b7fb9c 100644  --- a/section_Magneto_Gravity_Waves_In__.tex  +++ b/section_Magneto_Gravity_Waves_In__.tex 
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The same effect occurs for magneto-gravity waves that are reflected at $r_{\rm MG}$ rather than coupling with Alfven waves. The location of $r_{\rm MG}$ is a function of latitude, because the magnetic field cannot be spherically symmetric. Even in the simplest case of a purely dipolar magnetic field, the waves will scatter into a broad spectrum of \ell (\cite{Rincon_2003,Reese_2004}). In reality, purely poloidal fields are unstable, and the field will likely have a complex geometry containing both poloidal and toroidal components. An incoming $l=1$ wave is thus inevitably scattered into higher $\ell$ waves in the presence of a strong magnetic field. As described above, these waves cannot couple back to acoustic modes in the envelope, and remain trapped within the radiative core until they dissipate.  Finally, we note that magneto-gravity waves which are reflected at $r_{\rm MG}$ may be reflected onto the slow branch of magneto-gravity waves, since this branch has the same wavenumber as the fast branch at $r=r_{\rm MG}$. However, as the slow waves propagate back outward into regions with weaker magnetic fields, their wavenumber increases rapidly (see Figure \ref{fig:Prop}). The slow waves will thus dissipate very rapidly due to radiative diffusion or non-linear effects, the end result again being that they will not be observed as oscillations at the stellar surface.