A model of solar wind and corona driven by high-frequency Alfven waves

The small-scale ejection events in the solar atmosphere detected in recent space observations have been regarded as manifestations of small-scale magn etic reconnection. But such reconnections generate high-frequency Alfven wa ves. Based on this idea we set up a time-dependent, two-fluid model of coro nal heating and solar wind acceleration. Numerical solutions are made, show ing the time evolution, and including a discussion of their convergence and conservation properties. Under suitable assumptions regarding the generati on of the waves in the transition zone,the numerical solution can explain a number of observations including coronal heating, the radial density profi le of coronal holes, the acceleration of the wind near the bottom of the co rona and the high-velocity streams observed at 0.3 AU.