ACCELERATION AND HEATING OF 2-FLUID SOLAR-WIND BY ALFVEN WAVES

Earlier model studies of solar wind driven by thermal pressure and Alf ven waves have shown that wave amplitudes of 20-30 km s-1 at the coron al base are sufficient to accelerate the flow to the high speeds obser ved in quasi-steady streams emanating from large coronal holes. In thi s paper we focus on the energy balance in the proton gas and show that heat conduction from the region where the waves are dissipated may pl ay an important role in determining the proton temperature at the orbi t of Earth. In models with ''classical'' heat conduction we find a cor relation between high flow speed, high proton temperature, and low ele ctron temperature at 1 AU. The effect of wave heating on the developme nt of anisotropies in the solar wind proton gas pressure is also inves tigated in this study.