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Figure \ref{pvar_porb} shows two examples of how oscillation signatures vary. On the left are 10 RG/EBs with significant stellar activity detected during eclipses. Because the measured periods of variability are resonances of each system's orbital period, \citet{gau14} conclude that stellar activity is related to tidal interactions, which together inhibit oscillation strength. On the right is an example of the absence of oscillation modes. The Gaussian envelope of solar-like oscillations is clearly present in both blue power spectra, but strikingly absent in the black power spectrum.  \begin{figure}[h!]   \centering  \includegraphics[width=3.0in]{pvar_porb.png}  \includegraphics[width=3.4in]{oscillate_ornot.png}  \caption{A %\begin{figure}[h!]   %\centering  %\includegraphics[width=3.0in]{pvar_porb.png}  %\includegraphics[width=3.4in]{oscillate_ornot.png}  %\caption{A  hint of why some RG/EBs oscillate less than others. The left panel shows variability period (i.e., light curve variations due to star spots) verses orbital period. Larger symbols have higher amplitudes of stellar activity, and darker circles have stronger solar-like oscillations. Blue lines indicate resonances of $P_{\rm{var}}/P_{\rm{orb}}$. The right panel shows three power spectra for different RG/EBs, similar to those shown in Figure \ref{rainbowmodes}. The light blue has $\nu_{\rm{max}} \sim 4 \ \mu \rm{Hz}$ and the dark blue has $\nu_{\rm{max}} \sim 80 \ \mu \rm{Hz}$. However, the star with its power spectrum plotted in black clearly lacks solar-like oscillations. Figure from \citet{gau14}.} \label{pvar_porb}  \end{figure} %\label{pvar_porb}  %\end{figure}