Turbulence in the solar atmosphere and solar wind formation

Evolution of turbulent motions generated in subphotospherical layers at their propagation from the sun is studied. Turbulence in the photosphere, chramosphere and corona is investigated. The problem of forming energy fluxes and mass of solar wind is considered. Energy flux carried away by the solar wind is determined by energy flux Alfven waves. Energy transfer of Alfven waves by particles of the solar wind takes place at the distance r=10 R* from the Sun where R*-radius of the Sun. Mass flow of the solar wind is formed near the level of flow rate transition through the sonic rate (r approximately (2-4)R*)