deletions | additions       diff --git a/figures/DipoleEvolProp3/caption.tex b/figures/DipoleEvolProp3/caption.tex  index b696644..22d28a7 100644  --- a/figures/DipoleEvolProp3/caption.tex  +++ b/figures/DipoleEvolProp3/caption.tex 
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\label{fig:Prop}  {\bf Propagation Panel A: propagation  diagram for a magnetized red giant model. The model has $M = 1.6 \, M_\odot$, $R =6.6 \, R_\odot$, ${\nu}_{\rm max} = 120 \, {\rm {\mathrm{\mu}}Hz}$, and a core magnetic field of $\approx 6 \times 10^6 \,{\rm G}$ (see supplementary online material).} The red, blue, and green lines are the dipole Lamb frequency $L_1$, the buoyancy frequency $N$, and the magneto-gravity frequency $\omega_{\rm MG}$ (defined in equation \ref{eqn:maggrav}), respectively. Regions are colored by the types of waves they support: the red region is the acoustic wave cavity, the blue region is the magneto-gravity wave cavity, and the green region hosts only Alfven waves. The thick black line is the frequency of maximum power, $\nu_{\rm max}$, for this stellar model. Waves at this frequency behave like acoustic waves near the surface, magneto-gravity waves in the outer core, and Alfven waves in the inner core. {\bf Bottom:} Critical Panel B: critical  radial magnetic field strength, strength  $B_c$(equation \ref{eqn:Bc})  needed to suppress dipole oscillations, {\bf modes. We have  evaluated $B_c$ (equation \ref{eqn:Bc})  at the frequency  $\omega = 2 \pi \nu_{\rm max}$}. $B_c$ has a sharp minimum at the H-burning shell, which determines the minimum field strength $B_{c,{\rm min}}$ for dipole mode suppression.