deletions | additions       diff --git a/Magnetic Constraints.tex b/Magnetic Constraints.tex  index 68a0af3..c10231c 100644  --- a/Magnetic Constraints.tex  +++ b/Magnetic Constraints.tex 
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\end{equation}  Equation \ref{eqn:omc} should be evaluated at the H-burning shell, since the right hand side is typically maximized at this location. Modes with $\nu < \nu_c$ will be strongly suppressed, whereas modes with $\nu > \nu_c$ will not be. In stars at the border of suppression, with $\nu_{\rm max} \sim \nu_c$, lower frequency dipole modes will be suppressed, whereas higher frequency dipole modes will still be visible. These stars are especially useful because they allow for a measurement of $B$ at the H-burning shell via equation \ref{eqn:Bc}, evaluated at the observed value of $\omega_c = 2 \pi \nu_c$.  The early subgiant star KIC 8561221 analyzed by \cite{Garcia_2014} appears to show just such a transition. Using the approximate observed value of $\nu_c \approx 600 \, \mu{\rm Hz}$. We compute that the radial component of the magnetic field within the H-burning shell is $B \approx 1.5 \times 10^{7} \, {\rm G}$. The inferred field strength at the H-burning shell of KIC 8561221 is quite large, although it  could certainly be obtained if KIC 8561221 is the descendent of an 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 dipole pulsators found in \cite{Mosser_2011}. We therefore conclude that KIC 8561221 may be the descendant of a strongly magnetized Ap star, which managed to exhibit suppressed modes early on the RGB due to its strong field.