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Meredith L. Rawls added Background3.tex
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\subsection{Stellar Evolution in Binary Stars}
When stars of different mass form in a binary system, they are destined to evolve at different times. In close binaries, the situation can be dramatic: when one star expands to become a red giant, it can engulf its companion into a common envelope and affect the system's orbit, mass ratio, and ultimate fate. For the RG/EBs identified by \citet{gau13} and \citet{gau14}, however, such a history seems unlikely. These systems are all well detached; preliminary light curve modeling suggests that the sum of the two stars' radii never exceeds $\sim 30\%$ of the orbital semi-major axis.
On the other hand, many RG/EBs have eccentric orbits, as can be seen in Figure \ref{light_curves_all}. The five systems with the shortest periods appear to be synchronized in phase and in rotation with respect to the binary orbit, and have nearly circular orbits. This is unsurprising. In non-crowded environments, stars in a binary generally form at the same time, and evolve together. Given physical parameters such as mass, radius, and metallicity for an evolved red giant, and additional constraints on evolutionary stage from asteroseismology, it is possible to piece together a star's ``life story'' in the context of a binary system.
%\begin{figure}[h!]
%\centering
%\includegraphics[width=4.0in]{light_curves_all.png}
%\caption{\emph{Kepler} light curves for \citet{gau14}'s sample of RG/EBs, ordered from longest to shortest orbital period (top to bottom). Eccentric orbits, which appear as unevenly spaced primary and secondary eclipses, are clearly more prevalent for longer-period systems. The system names given in red are those which do not exhibit solar-like oscillations.}
%\label{light_curves_all}
%\end{figure}
