ACCELERATION OF THE HIGH-SPEED SOLAR-WIND

A theory is developed for the high speed solar wind based on a simple dissipation length characterization of wave heating of the coronal pla sma close to the Sun. It is shown that solutions with the correct part icle and energy fluxes and with a realistic magnetic field, match the requirements on the density at the base of the corona provided the dis sipation length is relatively small (similar to 0.25 - 0.5 solar radii ). The significant features of these solutions are that the accelerati on is rapid, with the sonic point at about 2 solar radii, and the maxi mum proton temperatures are high, namely 8 - 10 x 10(6) K, which could be consistent with some recent observations. Such efficient dissipati on requires any Alfven waves responsible to have frequencies in the ra nge 0.01 Hz - 10 kHz. This has implications for the nature of the plas ma and energy source in the chromospheric network.