deletions | additions       diff --git a/Magnetic Constraints.tex b/Magnetic Constraints.tex  index 4aa8d4b..330c111 100644  --- a/Magnetic Constraints.tex  +++ b/Magnetic Constraints.tex 
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%The critical field strength $B_c$ is dependent on wave frequency, and lower frequency waves are more susceptible to magnetic suppression.  For a given field strength, there is a transition frequency $\nu_c$ below which modes will be strongly suppressed and above which modes will appear normal. Stars which show this transition are especially useful because they allow for an {\bf inference} of $B$ at the H-burning shell via equation \ref{eqn:Bc}, evaluated at the transition frequency $\omega = 2 \pi \nu_c$. {\bf The RGB star KIC8561221 shows this transition (\cite{Garcia_2014}). \cite{Garcia_2014}.  Using the observed value of $\nu_c \approx 600 \, \mu{\rm Hz}$, we infer that the radial component of the magnetic field within the H-burning shell is $B \approx 1.5 \times 10^{7} \, {\rm G}$, although we cannot rule out the presence of stronger fields away from the H-burning shell}. This large field strength may indicate KIC8561221 is the descendant of a magnetic Ap star whose internal field was much stronger than the typical surface fields of $B \sim 3 \, {\rm kG}$ of Ap stars (\cite{Auri_re_2007}). \cite{Auri_re_2007}.     
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