Physical processes in the solar corona.

Contents: Transport theory (fundamental parameter regimes, the "ideal" problem, viscosity, parallel thermal energy transport, perpendicular transport, some comments on model building). Magnetohydrodynamic processes in the corona (equilibrium magnetic fields, linear stability and nonequilibrium, time-dependent phenomena). Energy and momentum balance of open and closed coronal structures (coronal holes and high-speed streams, Alfvén waves in the lower solar atmosphere, energy supply to magnetically closed coronal regions).