Formation and primary heating of the solar corona: Theory and simulation

An integrated magneto-fluid model, that accords full treatment to the veloc ity fields associated with the directed plasma motion, is developed to inve stigate the dynamics of coronal structures. It is suggested that the intera ction of the fluid and the magnetic aspects of plasma may be a crucial elem ent in creating so much diversity in the solar atmosphere. It is shown that the structures which comprise the solar corona can be created by particle (plasma) flows observed near the Sun's surface-the primary heating of these structures is caused by the viscous dissipation of the flow kinetic energy . (C) 2001 American Institute of Physics.