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Theories of stellar convective core overshoot can be examined throughanalysis of pulsating stars. Better accuracy can be achieved by obtainingexternal constraints such as those provided by observing pulsating stars ineclipsing binary systems, but this requires that the binary parameters beidentified so photometric variations of the pulsating component may be isolatedfrom the binary periodicity. This study aims to uncover the physical parametersof three binaries observed by the Kepler spacecraft. We also seek to evaluatethe feasibility of accurately constraining binaries using only readilyavailable time-series photometry and distance estimates. Binary models wereconstructed using the Physics of Eclipsing Binaries (PHOEBE) software package.Markov Chain Monte Carlo methods were used to sample the parameter space ofthese models and provide estimates of the posterior distributions for thesesystems. An initial run using binned light curve data was performed to identifygeneral parameter trends and provide initializing distributions for asubsequent analysis incorporating the full data set. We present theoreticalmodels for all three binaries, along with posterior distributions from our MCMCanalyses. Models for KIC 8314879 and KIC 10727668 produced a good match to theobserved data, while the model of KIC 5957123 failed to generate an appropriatesynthetic light curve. For the two successful models, we interpret theposterior distributions and discuss confidence in our parameter estimates anduncertainties. We also evaluate the feasibility of this procedure in variouscontexts, and propose several modifications to improve the success of futurestudies.

Using Computational Models to Uncover the Parameters of Three Kepler Binaries: KIC 5957123, KIC 8314879, and KIC 10727668