deletions | additions       diff --git a/Discussion.tex b/Discussion.tex  index f694279..6ccee10 100644  --- a/Discussion.tex  +++ b/Discussion.tex 
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%but we argue this is an unlikely explanation for most suppressed pulsators (see details in the supplementary material). Moreover the magnetic greenhouse effect makes a clear prediction: that for stars with frequency of maximum power similar to the critical magneto gravity frequency $\nu_{\rm c}$, dipole modes with $\nu >\nu_{\rm c}$ will be unaffected, while those with $\nu <\nu_{\rm c}$ should show suppression. KIC 8561221 displays this exact behavior, supporting the magnetic greenhouse mechanism.  Acore  magnetic field of amplitude $B > 10^4 \, {\rm G}$ (see Figure \ref{fig:Bc}) could be present in the core of  a red giant if it retains a fossil field from star formation, or if a convective core dynamo was at work during the main sequence. These strong fields may reside within the inner core with little external manifestation apart from the suppressed visibility of the dipole modes. However, fields of similar amplitude have been discussed in order to explain the suppression of thermohaline mixing in a small fraction of red giant stars, as inferred from the observations of their surface abundances \cite{Charbonnel_2007}. The calculated core field strength of $B_r \approx 1.5 \times 10^7 \, {\rm G}$ in KIC 8561221 shows very strong magnetic fields ($B \gg 10^6 \, {\rm G}$) can exist within the radiative cores of early RGB stars. Since these fields are likely inherited from previous stages of stellar evolution, slightly weaker ($B \gg 10^5 \,{\rm G})$ fields likely exist within the cores of some main sequence stars. %(sub-equipartition magnetic fields are easily above $B \sim 10^4 {\rm G}$).