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Several other works (\cite{Barnes_1998},\cite{Schecter_2001},\cite{MacGregor_2011},\cite{Mathis_2010},\cite{Mathis_2012},\cite{Rogers_2010},\cite{Rogers_2011}) have examined propagation of magneto-gravity waves in stellar interiors, focusing primarily on the solar tachocline. Remarkably, all of these works have considered a purely toroidal (horizontal) magnetic field configuration, because they were motivated by the strong toroidal field though to exist due to the shear flows in the solar tachocline. However, horizontal fields must be stronger by a factor $N/\omega \gg 1$ in order to strongly affect gravity waves. Consequently, these works have missed the extremely important effect of {\it radial} magnetic fields on gravity wave dynamics, which generally requires much smaller field strengths to become important.  A few papers have attempted the difficult task of calculating the oscillation mode spectra of magnetized stars (\cite{Rincon_2003},\cite{Reese_2004},\cite{Lee_2007},cite{Lee_2010}). Unfortunately, the complexity of the results makes their interpretation challenging. WE emphasize that simple field configurations seem to allow for a continuum of Alfvenic modes. Additionally, the modes generally have complex angular structures and are composed of a broad spectrum of spherical harmonics. This reinforces our claim that strong fields will scatter waves into a wide range of $\ell$ values.