In this study, we look specifically at binary white dwarfs where the companion is a main sequence star. In particular, we look at very hot white dwarfs, many of which demonstrate the "hydrogen problem" in which modeling of their hydrogen absorption features, and optical features in general, do not appear to give accurate temperatures. The two systems presented in this study, WD1136+667 and Gaia-DR2-3150, were modeled using the PHOEBE code to determine the masses, radii, and temperatures of the two stars along with the inclination of the binary and stellar separation. While these models are integral as a first step in our understanding, this is only the first step of a more extensive FUV Hubble Space Telescope program examining very hot white dwarfs. One goal is to compare temperatures determined from UV spectra to those determined kinematically from binary models such as the preliminary models presented here.