deletions | additions       diff --git a/figures/DipoleBEvolNew3/caption.tex b/figures/DipoleBEvolNew3/caption.tex  index 14bd02c..0f20504 100644  --- a/figures/DipoleBEvolNew3/caption.tex  +++ b/figures/DipoleBEvolNew3/caption.tex 
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\label{fig:Bc}  {\bf Panel A: Minimum field strength $B_{c,{\rm min}}$ required for magnetic suppression of dipole oscillation modes in stars evolving up the RGB.} Values of minimum field strength are shown as a function of the frequency of maximum power, $\nu_{\rm max}$, for stars of different mass. The value of $B_{c,{\rm min}}$ has been computed for modes with frequency $\nu = \nu_{\rm max}$. We have labeled the observed value of $\nu_{\rm max}$ and {\bf inferred} core field strength $B$ for the lower RGB star KIC8561221 \cite{Garcia_2014} and a lower limit to the field strength in KIC9073950.The bends at the top of the panel occur at the base of the RGB, while the hooks in the lower right corner occur at the luminosity bump.  {\bf Panel B:} Asteroseismic HR diagram showing stellar evolution tracks over the same range in $\nu_{\rm max}$. Stars evolve from left to right as they ascend the RGB. Dashed lines show the end of main sequence evolution, thin solid lines are the sub-giant phase, and thick solid lines are the RGB. We do not show any evolution beyond the RGB (i.e., no clump or asymptotic giant branch).