deletions | additions       diff --git a/figures/DipoleBEvolNew3/caption.tex b/figures/DipoleBEvolNew3/caption.tex  index dfe1532..d6dd094 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 %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 core  field strength $B$ for the lower RGB star KIC 8561221 (\cite{Garcia_2014}) and a lower limit to the field strength in KIC 9073950. The bends at the top of the panel occur at the base of the RGB (at the end of the subgiant phase), RGB,  while the hooks in the lower right corner occur at the luminosity bump. {\bf Bottom:} Corresponding 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 evolution, thin  solid lines are the sub-giant phase,defined as the period between core hydrogen depletion  andthe maximum in $\nu_{\rm max}$ at the base of the RGB, which is shown in  thick solid lines. lines are the RGB.  We do not show any evolution beyond the RGB (i.e., no clump or asymptotic giant branch).