A Selfconsistent Turbulent Model for Solar Coronal Heating
Abstract
The rate of solar coronal heating induced by the slow random motions of the dense photosphere is calculated in the framework of an essentially parameterfree model. This model assumes that these motions maintain the corona in a state of smallscale MHD turbulence. The associated dissipative effects then allow a largescale stationary state to be established. The solution for the macroscopic coronal flow and the heating flux is first obtained assuming the effective (turbulent) dissipation coefficients to be known. In a second step these coefficients are calculated by the selfconsistency argument that they should result from the level of turbulence associated with this very heating flux. For the sake of tractability the derivation is restricted to a twodimensional situation where boundary flows are translationally symmetric. The resulting value of the heating rate and the predicted level of microturbulent velocity compare satisfactorily with the observational data.
 Publication:

The Astrophysical Journal
 Pub Date:
 May 1992
 DOI:
 10.1086/171280
 Bibcode:
 1992ApJ...390..297H
 Keywords:

 Magnetohydrodynamic Turbulence;
 Plasma Heating;
 Solar Corona;
 Turbulence Models;
 Heat Flux;
 Hydrodynamic Equations;
 Magnetohydrodynamic Flow;
 Photosphere;
 Solar Physics;
 MAGNETOHYDRODYNAMICS: MHD;
 SUN: CORONA;
 TURBULENCE