Previous wave-driven solar wind models (Hollweg, 1978) have been extended by including a new hypothesis for the nonlinear wave dissipation. The hypothesis is that the waves dissipate via a turbulent cascade at the rate given by (1) and the waves evolve according to (16). A subhypothesis is that the relevant correlation length scales as the distance between magnetic field lines. This hypothesis allows us to treat the corona and the solar wind on an equal footing; unlike in previous wave-driven models, we do not assume that the coronal heating takes place below the base of the model. The models exhibit the correct qualitative features, viz., a steep temperature rise (the transition region) to a maximum coronal temperature in excess of 106K, and a substantial solar wind mass flux in excess of 3.5¿108 cm-2 s-1 at 1 AU. However, the model fails in detail. Parameters that yield a high-speed flow at 1 AU have base pressures that are too low; parameters that yield correct base pressures have low solar wind flow speeds. However, the model ''comes close.'' Thus although we have not shown that the initial hypothesis is consistent with available data, we feel that there are sufficient uncertainties both in the model and in the data to preclude outright rejection of the hypothesis altogether.