deletions | additions       diff --git a/Abstract.tex b/Abstract.tex  index fbb5190..d4fa5fc 100644  --- a/Abstract.tex  +++ b/Abstract.tex 
...
\begin{abstract} %\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 ($M_1 = 2.16 \pm 0.04\ M_{\odot}, M_2 = 2.14 \pm 0.03\ M_{\odot}$) and radius ($R_1 = 7.90 \pm 0.04 \ R_{\odot}, R_2 = 8.33 \pm 0.04 \ R_{\odot}$) 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 and radius ($M_{\rm{seismo}} = 2.06 \pm 0.13 \ M_{\odot}, R_{\rm{seismo}} = 8.10 \pm 0.18 \ R_{\odot}$). It is unlikely that two sets of solar-like oscillations lie on top of one another, because the predicted difference in oscillation peak frequencies for these nearly-identical stars is larger than the frequency resolution. 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} %\end{abstract}  \keywords{binaries: eclipsing --- methods: data analysis --- stars: fundamental parameters --- stars: AGB and post-AGB --- stars: oscillations (including pulsations)}