deletions | additions       diff --git a/subsection_Magneto_Gravity_Waves_The__.tex b/subsection_Magneto_Gravity_Waves_The__.tex  index 917cb43..96747b4 100644  --- a/subsection_Magneto_Gravity_Waves_The__.tex  +++ b/subsection_Magneto_Gravity_Waves_The__.tex 
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Several previous works \cite{Barnes_1998,Schecter_2001,MacGregor_2011,Mathis_2010,Mathis_2012,Rogers_2010,Rogers_2011} have examined the propagation of magneto-gravity waves in stellar interiors, focusing primarily on the solar tachocline. However, all of these works have considered a purely toroidal (horizontal) magnetic field configuration, because they were motivated by the strong toroidal field thought to exist due to the shear flows in the solar tachocline. Horizontal fields must be stronger by a factor $k_r/k_\perp \sim N/\omega \gg 1$ in order to strongly affect gravity waves. Consequently, these works did not examine the extremely important effect of radial magnetic fields on gravity wave dynamics.  {\bf Finally, many papers (e.g., \cite{Saio_2014,Saio_2012,Dziembowski_1996,Cunha_2000,Cunha_2006,Campbell_2006,Sousa_2008} \cite{Dziembowski_1996,Cunha_2000,Cunha_2006,Campbell_2006,Sousa_2008,Saio_2012,Saio_2014}  have examined the effect of magnetic fields on the acoustic oscillations of rapidly oscillating Ap stars. In this case, the magnetic field strongly affects the acoustic waves only near the surface of the star where the magnetic pressure becomes comparable to the gas pressure. These authors reach similar conclusions to those discussed below: some wave energy can be lost by transmission into Alfven waves, and the geometry of the magnetic field is important. However, the oscillation modes in these stars indicates that observable modes can still exist in the presence of strong magnetic fields, and future studies should further examine possible connections between the physics of oscillating Ap stars and red giants with magnetic cores.  }