deletions | additions       diff --git a/subsection_Magneto_Gravity_Waves_The__.tex b/subsection_Magneto_Gravity_Waves_The__.tex  index 388f1cf..fe38a0d 100644  --- a/subsection_Magneto_Gravity_Waves_The__.tex  +++ b/subsection_Magneto_Gravity_Waves_The__.tex 
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In the solar atmosphere, the fate of magneto-gravity-acoustic waves propagating upward into the chromosphere is largely determined by the geometry of the magnetic field. \cite{Newington_2009} and \cite{Newington_2011} demonstrate that mostly radial fields tend to reflect waves downward at the effective value of $r_{\rm MG}$ in the solar atmosphere. Moreover, the waves are reflected onto the slow branch, i.e., they transition into Alfven waves as they propagate downward. We suspect the same process will occur in stellar interiors: ingoing waves will mostly reflect at $r_{\rm MG}$ and will then transition into Alfven waves as they propagate back outward. Sufficiently horizontal fields will allow more wave transmission into Alfven waves in the core, however, stronger fields are required in this case.  Reflected The reflected  waves will dissipate much faster than the incident  dipole waves, preventing them from ever tunneling back to the surface. Waves reflected back onto the fast branch will have higher $\ell$, shorter wavelengths, and will damp out more quickly than dipole waves. Waves reflected onto the slow branch have wavenumbers orders of magnitude larger than the fast branch of magneto-gravity waves (see Figure \ref{fig:Prop2}) as they propagate outward into weakly magnetized regions. Therefore, any wave energy reflected into slow magneto-gravity waves will be quickly dissipated via radiative diffusion.