2011AJ....142...50F

Exoplanet transit and Doppler surveys discover many binary stars during their operation that can be used to conduct a variety of ancillary science. Specifically, eclipsing binary stars can be used to study the stellar mass-radius relationship and to test predictions of theoretical stellar evolution models. By cross-referencing 24 binary stars found in the MARVELS Pilot Project with SuperWASP photometry, we find two new eclipsing binaries, TYC 0272-00458-1 and TYC 1422-01328-1, which we use as case studies to develop a general approach to eclipsing binaries in survey data. TYC 0272-00458-1 is a single-lined spectroscopic binary for which we calculate a mass of the secondary and radii for both components using reasonable constraints on the primary mass through several different techniques. For a primary mass of M₁= 0.92±0.1 M _☉, we find M₂= 0.610±0.036 M_☉, R₁= 0.932±0.076 R _☉, and R₂= 0.559±0.102 R_☉, and find that both stars have masses and radii consistent with model predictions. TYC 1422-01328-1 is a triple-component system for which we can directly measure the masses and radii of the eclipsing pair. We find that the eclipsing pair consists of an evolved primary star (M₁= 1.163±0.034 M_☉, R₁= 2.063 ± 0.058 R_☉) and a G-type dwarf secondary (M₂= 0.905±0.067 M_☉, R₂= 0.887±0.037 R_☉). We provide the framework necessary to apply this analysis to much larger data sets.