MODELING OF A SOLAR CORONAL LOOP

Montgomery end co-workers have developed a framework to describe the s teady state of a turbulent magnetofluid, without the usual recourse to linearization. Thus the magnetic and velocity fields emerge in their fully nonlinear form as a consequence of the selective decays of the i nvariants of the system. Using this statistical theory of magnetohydro dynamic turbulence, the pressure, magnetic and flow fields of a solar coronal loop have been determined. The spatial and time profiles of th e loop pressure are derived. A comparison with the observed properties of the loops is made, whenever possible.