deletions | additions       diff --git a/Conclusion.tex b/Conclusion.tex  index c2b3872..ebe8d11 100644  --- a/Conclusion.tex  +++ b/Conclusion.tex 
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The two stars in KIC 9246715 are nearly twins ($M_1 = 2.16 \pm 0.04\ M_{\odot}$, $M_2 = 2.14 \pm 0.03\ M_{\odot}$, $R_1 = 7.90 \pm 0.04 \ R_{\odot}$, $R_2 = 8.33 \pm 0.04 \ R_{\odot}$), yet we observe only one pair of solar-like oscillations ($M = 2.17 \pm 0.13 \ M_{\odot}$, $R = 8.26 \pm 0.16 \ R_{\odot}$). We find that the oscillations are most likely from Star 2, the larger and cooler of the pair, which may also be less magnetically active than Star 1. Surface gravities from photodynamic modeling ($\log g_1 = 2.977 \pm 0.004$, $\log g_2 = 2.927 \pm 0.003$) and asteroseismology ($\log g = 2.942 \pm 0.007$) nearly agree, while the surface gravity from stellar atmosphere modeling is higher ($\log g_1 = 3.21 \pm 0.45$, $\log g_2 = 3.33 \pm 0.37$). A similar discrepancy was found in a population study comparing asteroseismic and spectroscopic surface gravities \citep{hol15}, but the physical cause is uncertain.  The stars in KIC 9246715  were born and evolved together, but the present evolutionary state (red giant branch vs. red clump) is unclear. Tidal circularization timescales and radii from a stellar evolution model indicate that both stars should be on the red giant branch with an age of $7.28 \times 10^8$ years, while the oscillation mode period spacing---which is difficult to measure due to a weak and noisy oscillation spectrum---suggests the oscillating star may be on the red clump. Future work will examine this disagreement in more detail with precise ``peak-bagging'' of individual oscillation modes. Red giants are ideal beacons for probing the Milky Way Galaxy via asteroseismology, so it is crucial that we understand the accuracy and precision of asteroseismically-derived physical parameters. Along the same lines, more than half of cool stars should be in binary or multiple systems, so galactic studies must be done carefully due to external influences of binarity on solar-like oscillations. Detailed studies of the handful of known RG/EBs are crucial to ensure we understand these galactic beacons. Future work will characterize the other 14 known oscillating RG/EBs as well as several non-oscillating RG/EBs. These have the potential to become some of the best-studied stars while simultaneously helping us better understand the structure of the Milky Way.