We consider the possibility that the heating of the corona and the heating and acceleration of the solar wind can be described by a single process, namely, the turbulent dissipation of solar-generated Alfven waves at the Kolmogorov rate. The model assumes that Te=Tp in r≤2 RS but drops electron-proton coupling in r>2 Rs. The dissipated wave energy is assumed to heat only the protons. Classical heat conduction is used in r>10 RS, and an electron polytrope is used in r>10 RS. The models have the right qualitative features: a steep temperature rise to T>106 K and acceleration to supersonic speeds. But models with base pressures neT>2¿1014 (cgs) are too slow: v(1 AU)400 km s-1 have lower base pressures: 1014<neT<2¿1014 (cgs). A difficulty with the model is that line-of-sight proton random velocities (thermal plus wave) are larger than values deduced from Lyman &agr; resonant scattering observations in 1.5≤r/RS≤4, and they do not fall off with r to the extent observed. Large random velocities are due in part to a proton temperature peak at r≈3--4 Rs. On the whole, this model seems unsatisfactory, but several possible resolutions are discussed. ¿ American Geophysical Union 1988