The effects of induced scattering of Alfven waves for the solar wind acceleratio

Abstract

The analysis of energy balance of coronal holes gives that to accelerate the fast solar wind streams the energy flux of the order of 800 erg/cm$^2$ s is needed. Axford and McKenzie suggested that the energy source, necessary to accelerate fast solar wind, is in the regions of strong magnetic field that define the boundaries of chromospheric supergranules. If the magnetic field is not strictly unipolar in these regions, the necessary energy is released in the processes of impulsive reconnection events. For the plasma parameters appropriate for the coronal base such processes of impulsive reconnection are accompanied by the generation of Alfven and fast magnetosonic waves with the period of the order of 1 s. On the basis of kinetic equation the model for the evolution of Alfven waves in solar wind is suggested. The induced scattering of these waves by plasma ions is considered as the dominant mechanism of dissipation of Alfven waves. The description of the evolution of the wave spectra in the process in the processes of their propagation till the distance of 187 solar radii was found.