Hot, luminous OB stars have strong stellar winds driven by the line-scattering of the star's continuum radiation. This line-driving mechanism is understood to be highly unstable to small scale perturbations. I review efforts to simulate the nonlinear evolution of this instability using radiation hydrodynamics simulation codes. Because the usual local, Sobolev treatment for the line-force does not apply, a major challenge has been to develop computationally tractable methods for approximating the inherently non-local radiative transfer in the large number of wind-driving lines. Results of 1-D simulations generally show development of a highly compressible, stochastic wind structure dominated by strong reverse shocks and dense shells; these arise from amplification of inward-propagating radiatively-modified acoustic modes with anticorrelated velocity and density. In 2-D and 3-D, linear analysis predicts that lateral variations in velocity should be strongly damped by the “line-drag” effect of the diffuse radiation scattered within the line resonance, suggesting possible suppression of classical Rayleigh-Taylor modes for lateral breakup of wind structure. This motivates current efforts toward 2-D simulation of the nonlinear wind structure. An overall goal is to develop connections with studies of highly compressible turbulent structure in other physical and astrophysical contexts.