  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 M_1 =
0.92 +/- 0.1 M_solar, we find M_2 = 0.610 +/- 0.036 M_solar, R_1 = 0.932 +/-
0.076 R_solar and R_2 = 0.559 +/- 0.102 R_solar, 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 (M_1 = 1.163 +/- 0.034 M_solar, R_1 = 2.063 +/- 0.058 R_solar) and
a G-type dwarf secondary (M_2 = 0.905 +/- 0.067 M_solar, R_2 = 0.887 +/- 0.037
R_solar). We provide the framework necessary to apply this analysis to much
larger datasets.
