deletions | additions       diff --git a/Discussion.tex b/Discussion.tex  index fa02b43..be166ba 100644  --- a/Discussion.tex  +++ b/Discussion.tex 
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\subsection{Comparison with asteroseismology}\label{seismo}  Because both stars We expect the evolved giants  in KIC 9246715are evolved giants with convective envelopes, we expect both  to exhibit solar-like oscillations (I THINK YOU'RE SAYING THIS FOR THE THIRD TIME ... REALLY? WHERE ARE THE FIRST TWO? SEEMS LIKE RELEVANT CONTEXT TO ME -MR). oscillations.  These should be observable as p-modes for radial oscillations and mixed p- and g- modes for dipolar and quadrupolar oscillations in \emph{Kepler} long-cadence data. For solar-like oscillators, the average large frequency separation of p-modes $\Delta \nu$ has been shown to scale with the square root of the mean density of the star, while the frequency of maximum oscillation power $\nu_{\rm{max}}$ carries information about the physical conditions near the stellar surface and is a function of surface gravity and temperature \citep{cha13}. These scaling relations may be used to estimate a star's density and surface gravity: \begin{equation} \label{density}  {\left( \frac{\rho}{\rho_{\odot}} \right)} \simeq {\left( \frac{\Delta \nu}{\Delta \nu_{\odot}} \right)}^{2} 
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We find that the masses, radii, and surface gravities for both stars in KIC 9246715 are all consistent with the asteroseismic values, so we unfortunately cannot use KIC 9246715 to draw conclusions about the accuracy of the scaling relations. A comparison of key parameters determined from our different modeling techniques is in Table \ref{table2}. We speculate on which star is the oscillator and further explore the binary's co-evolutionary history in Section \ref{context}.  We can say that the oscillating star, whichever it may be, is a core-helium-burning star on the red clump. WRITE ABOUT HOW WE KNOW THIS BECAUSE MIXED MODES. DISCREPANCY WITH MESA RADIUS RESULTS??