deletions | additions       diff --git a/figures/DipoleStruc/caption.tex b/figures/DipoleStruc/caption.tex  index b48d3aa..b8955c9 100644  --- a/figures/DipoleStruc/caption.tex  +++ b/figures/DipoleStruc/caption.tex 
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\label{Fig:Struc}  {\bf Top:}  Structure of the $M=1.6 M_\odot$ stellar model shown in Figure \ref{fig:Prop}. At this stage of evolution, the star has a $\sim \! 0.2 M_\odot$ He core, surrounded by a $\sim \! 0.1 M_\odot$ radiative outer core. The bulk of the mass and radial extent of the star is comprised by the thick convective envelope. We have also added a simple magnetic {\bf Bottom:} Magnetic  field to the radiative core of the star, calculated by assuming magnetic flux conservation from a dipole field on the main sequence. Even though the main sequence dipole field was conservatively capped at $30 \, {\rm kG}$ within the interior, field strengths of $B \gtrsim 1 \, {\rm MG}$ are easily attainable within the cores of red giants. The We also plot the  criticalmagnetic  field $B_c$ from equation \ref{eqn:Bc} has a sharp minimum at as in Figure \ref{fig:Prop}. Because $B>B_c$ in  the H-burning shell, corresponding to core of this stellar model,  theminimum field required for  magnetic suppression. greenhouse effect may occur.