deletions | additions       diff --git a/abstract.tex b/abstract.tex  index c5f8fb3..de4303f 100644  --- a/abstract.tex  +++ b/abstract.tex 
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%\begin{abstract}  We combine \emph{Kepler} photometry with ground-based radial velocities to present a comprehensive photodynamical model for the double red giant eclipsing binary KIC 9246715. The two stars are nearly identical in mass ($M_1 = 2.16 \pm 0.04\ M_{\odot}$, $M_2 = 2.14 \pm 0.03\ M_{\odot}$), M_{\odot}$) and  radius ($R_1 = 7.90 \pm 0.04 \ R_{\odot}$, $R_2 = 8.33 \pm 0.04 \ R_{\odot}$), and surface gravity (PUT SURFACE GRAVITIES HERE) R_{\odot}$)  in a well-separated and eccentric ($e = 0.35$) 171-day orbit, yet an asteroseismic analysis identifies only a single set of solar-like oscillations. The oscillation amplitudes are weaker than expected from similar red giants. Because the two stars are nearly twins, KIC 9246715 is not a good target for precisely testing the asteroseismic scaling relations---both stars are consistent with the single inferred mass, radius, mass  and surface gravity radius  ($M_{\rm{seismo}} = 2.06 2.21  \pm 0.13 \ M_{\odot}$, $R_{\rm{seismo}} = 8.10 8.30  \pm 0.18 0.16  \ R_{\odot}$, PUT SEISMIC LOG G HERE). $\log g = 2.944 \pm 0.007$). EDIT THIS TO SAY STAR 2 IS PROBABLY THE OSCILLATOR BUT WE CAN'T SAY FOR SURE.  We suspect stellar activity or modest tidal forces are responsible for a lack of solar-like oscillations in one star and weak oscillations in the other. We further show that KIC 9246715 is a coeval binary with both stars in the Helium-core-burning red clump. This system is a useful asteroseismic case study and paves the way for a detailed analysis of more red giants in eclipsing binaries. %\end{abstract}