Alfvenic turbulence and wave propagation in the corona and heliosphere

The properties of Alfven wave propagation through the solar corona and heliosphere are reviewed, with particular emphasis on the role of large scale radial gradients in determining the variation of amplitude with distance. Some comments on the role of photospheric vorticity as a source for Alfven waves are presented, 1-D and 2-D MHD couplings of the waves as they climb out of the coronal density gradient are described (parametric decay, sound wave generation), while the final section is devoted to the 1-D propagation of Alfven type solitons in the solar wind. Throughout, the focus is on the relevance of theory to the turbulent fluctuations measured in the wind and remote sensing observations of the corona: many puzzles and problems are highlighted.