ABSTRACT This is a study of solar and solar wind magnetohydrodynamics (MHD). Four basic areas will be emphasized; (1) coronal processes of 3D reconnection, (2) Alfven wave absorption and turbulence, (3) instability and turbulence in coronal mass ejections, and (4) the theory of fast dynamo action and the modelling of the alpha-effect. These problems are important for understanding flares, coronal heating, the solar wind and the solar cycle. Earlier work concentrated on ideal and resistive MHD instabilities in line-tied solar coronal loops, and showed, in nonlinear MHD simulations, that the instabilities cause current sheets to form. Also studied was Alfven wave resonant absorption in coronal flux tubes driven by photospheric motion. The current work will concentrate on current sheets, 3D reconnection, and possible singularities of 3D equilibria in solar coronal magnetic loops. Secondary Kelvin-Helmholtz instabilities in Alfven waves and other absorption mechanisms will also be studied. MHD instabilities and dynamics of coronal mass ejection models will be investigated, and the fast dynamo analyses will be expanded to encompass steady flows with chaotic webs, and time dependent flows which are close to integrable flows. The effort will include new methods for calculating transport by chaotic flow, and the graphical representation of magnetic structures produced by dynamos. *** //
