deletions | additions       diff --git a/figures/DipoleBEvolNew3/caption.tex b/figures/DipoleBEvolNew3/caption.tex  index 2d49a3a..afb8b53 100644  --- a/figures/DipoleBEvolNew3/caption.tex  +++ b/figures/DipoleBEvolNew3/caption.tex 
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\label{fig:Bc}  {\bf Top:} Minimum field strength $B_{c,{\rm min}}$ required for magnetic suppression of dipole oscillation modes in stars evolving up the RGB, as a function of their frequency of maximum power, $\nu_{\rm max}$. The value of $B_{c,{\rm min}}$ has been computed for modes with frequency $\nu = \nu_{\rm max}$. A star observed to have suppressed dipole modes has a minimum field strength of $B_{c,{\rm min}}$ within its core. We have labeled the observed value of $\nu_{\rm max}$ and calculated field strength $B$ for the lower RGB star stars  KIC 8561221 (\cite{Garcia_2014}). (\cite{Garcia_2014}) and KIC 9073950.  The bends at the top of the panel occur at the base of the RGB (at the end of the sub-giant branch), phase),  while the hooks in the lower right corner occur at the luminosity bump. {\bf Bottom:} Corresponding asteroeismic 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 branch, phase,  defined as the period between core hydrogen depletion and the maximum in $\nu_{\rm max}$ at the base of the RGB, which is shown in thick solid lines. We do not show any evolution beyond the RGB (i.e., no clump or asymptotic giant branch).