deletions | additions       diff --git a/Magnetic Constraints.tex b/Magnetic Constraints.tex  index 14f58fe..5d984fe 100644  --- a/Magnetic Constraints.tex  +++ b/Magnetic Constraints.tex 
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\end{equation}  where $\omega_{\rm vis}$ is the lowest frequency observable mode with approximately normal amplitude.  The early subgiant star KIC 8561221 analyzed by \cite{Garc_a_2014} appears to show just such a transition. We construct a Mesa model of the star with similar parameters to those found by \cite{Garc_a_2014}, and evaluate equation \ref{eqn:BH} using the approximate observed value of $\nu_{\rm vis} \approx 600 \, \mu{\rm Hz}$. We find $B_H \approx 7 \times 10^{6}$ 10^{6} \, {\rm G}$  for this star. The inferrred field strength at the H-burning shell of KIC 8561221 is quite large, although could certainly be obtained if KIC 8561221 is the descendent of a roAp star or a very magnetic Ap star with a surface field strength of $\sim 10 \, {\rm kG}$, near the upper end of the distribution found by \cite{Auri_re_2007}. Indeed, KIC 8561221 is somewhat of an outlier in the population of red giants with suppressed dipole modes, as its $\nu_{\rm max}$ is larger than any of the suppressed deipole pulsators found in \cite{Mosser_2011}. We therefore conclude that KIC 8561221 is the descendant of a strongly magnetized Ap star, which managed to exhibit suppressed modes early on the RGB due to its strong field. Most magnetic stars with somewhat weaker fields likely do not exhibit suppressed dipole modes until later on the RGB where the critical field strength $B_c$ has fallen (see Figure \ref{fig:DipoleBEvol}) to more commonly attained values.