deletions | additions       diff --git a/figures/DipoleProp/caption.tex b/figures/DipoleProp/caption.tex  index 7108fdf..09076d4 100644  --- a/figures/DipoleProp/caption.tex  +++ b/figures/DipoleProp/caption.tex 
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\label{fig:Prop}  {\bf Top:} Propagation diagram for a $M=1.6 \,M_\odot$, $R=7.3 \,R_\odot$, $\nu_{\rm max}=100 \,\mu{\rm Hz}$ RGB stellar model with a magnetized core. The red, blue, and green lines are the dipole Lamb frequency $L_1$, the Brunt-Vaisala frequency $N$, and the magneto-gravity frequency $\omega_{MG}$ (defined in equation \ref{eqn:maggrav}), respectively. The black line is the angular frequency of maximum power, $\omega_{\rm max}$. For a wave with $\omega=\omega_{\rm max}$, the labeled shaded regions indicate the nature of the wave in different regions of the star. {\bf Bottom:} Critical radial magnetic field strength, $B_c$ (equation \ref{eqn:Bc}) needed to suppress dipole oscillation modes.In red giants,  $B_c$ has a sharp minimum at the H-burning shell, which determines the minimum field strength $B_{c,\rm {min}}$ for dipole mode suppression. %{\bf Middle:} Sound speed, $v_s$, gravity wave radial group velocity, $v_{g,r}$ (for $\omega=\omega_{\rm max}$), and Alfven velocity, $v_A$, as a function of radius. Waves travel at a group velocity of $v_s$, $v_{g,r}$, and $v_A$ for acoustic, gravity, and Alfven waves, respectively. {\bf Bottom:} Radial wave number, $k_r$, for a wave with $\omega=\omega_{\rm max}$, as a function of radius. We have plotted the wavenumbers of acoustic waves (p-waves), fast magneto-gravity waves (mg-waves), slow magneto-gravity waves (slow-waves), and Alfven waves (a-waves). The dashed blue line shows the wavenumber for gravity waves (g-waves) in the absence of a magnetic field.