Binary stars are the primary source of our knowledge of the fundamental properties of stars. They are excellent laboratories for testing our understanding of the structure and evolution of stars, as well as stellar dynamics, composition, and age. While most stars are believed to exist in binary or multiple systems, a large fraction of these systems result in one star eclipsing another. In such cases, a complete understanding of the properties of each star and the system as a whole can be ascertained. Overcontact binaries, where stars are close enough to share their stellar atmosphere, are especially valuable laboratories when examining stellar convection, magnetic fields, and gravitational waves. 

Preliminary analyses of close eclipsing binary systems are presented. Calibration and photometry are completed using AstroImageJ, leading to a light curve. Modeling is completed through the newest version of the PHysics Of Eclipsing BinariEs (PHOEBE) software. Best-fit stellar models are determined, which provide observational constraints on the physical parameters of the system and each component. In some cases, stellar spots are required to represent surface phenomena. Each model is rigorously examined across multiple dimensions in a Markov Chain Monte Carlo process in order to determine the uniqueness of the model and to determine the model’s uncertainties. This research makes use of the BigRed200 High-Performance Computing system.