  In this paper we show how the formalism of Wu & Goldreich developed for
weakly nonlinear white dwarf pulsations can be extended to the fully nonlinear
case. Due to the computational simplification this affords over the simulations
of Brickhill (1992) and Ising & Koester (2001), we are able to obtain the first
ever fits of observed light curves. These fits allow us to obtain not only mode
identifications but also to constrain the average depth of the convection zone
and its sensitivity to changes in effective temperature. We are thus able to
probe the fundamental physics of convection in these objects.
