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In principle, it is possible that another symmetry-breaking mechanism within the core could suppress dipole mode amplitudes. The only other plausible candidate is rapid core rotation. In order for rotation to strongly modify the incoming waves such that they will be trapped in the core, the core must rotate at a frequency comparable to $\nu_{\rm max}$, roughly two orders of magnitude faster than the values commonly measured in red giant cores \cite{Beck_2011,Mosser_2012,deheuvels_2014}. The depressed dipole mode star KIC8561221 \cite{Garcia_2014} does not exhibit rapid core rotation and disfavors the rotation scenario.  A magnetic field of amplitude $B \! > \! 10^4 \, {\rm G}$ (see Fig. \ref{fig:Bc}) could be present in the core of a red giant if it was retained from previous phases of stellar formation/evolution \cite{supplementary}. (supplementary material).  These strong fields may reside within the inner core with little external manifestation apart from the reduced 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 inferred core field strength of $B_r \! \gtrsim \! 1.5 \! \times \! 10^7 \, {\rm G}$ in KIC8561221 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 could exist in the cores of exceptional very highly magnetized main sequence stars.