deletions | additions       diff --git a/Discussion.tex b/Discussion.tex  index 7b1ce07..18275b8 100644  --- a/Discussion.tex  +++ b/Discussion.tex 
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%{\left( \frac{M}{M_\odot} \right)} \simeq {\left( \frac{\nu_{\rm{max}}}{\nu_{\rm{max, \ \odot}}} \right)}^{3} {\left( \frac{\Delta \nu}{\Delta \nu_\odot} \right)}^{-4} {\left( \frac {T_{\rm{eff}}} {T_{\rm{eff, \ \odot}}} \right)}^{1.5}.  %\end{equation}  The asteroseismic mass and surface gravity are consistent with those from the ELC model for both stars, while the asteroseismic radius is only consistent with Star 2 (Table \ref{table2}). Neither star's mean density agrees with the asteroseismic value, but Star 2 is much closer than Star 1. Overall, our asteroseismic analysis suggests the oscillating star is Star 2. However, we cannot definitely conclude this without considering the temperature dependence of the scaling relations. From \citet{gau13}, \citet{gau14}, and the present work, asteroseismic masses and radii were reported to be $(1.7 \pm 0.3 M_\odot, 7.7 \pm 0.4 R_\odot)$ and $(2.06 \pm 0.13 M_\odot, 8.10 \pm 0.18 R_\odot)$, and now we have $(2.21 \pm 0.12 M_\odot, 8.30 \pm 0.16 R_\odot)$. Among these, $\nu_{\rm{max}}$ does not vary much (102.2, ($102.2,  106.4,and  106.4 $\mu\rm{Hz}$ \ \mu\rm{Hz}$  respectively) while $\Delta \nu$ varies even less (8.3, ($8.3,  8.32, 8.31 $\mu$Hz), \ \mu\rm{Hz}$),  while the assumed temperatures were 4699 K (from the KIC), 4857 K (from \citet{hub14.2}), and 5050 K (present work JUSTIFY THIS TEMP CHOICE??). Even if temperature is the least influential parameter on stellar masses and radii in the asteroseismic scalings, we are at a level of precision where errors on temperature dominate the global asteroseismic results. This is also because of the temperature dependence that asteroseismic scalings better match mean density than surface gravity. %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}. 
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