The origin of solar flares
Abstract
Observations indicate that solar flares have a turbulent origin and that there is insufficient time for full development of the spectrum corresponding to the linear eigenfunction perturbations. We propose therefore to study the problem expanding the perturbations on a basis of general functions which are not necessarily eigenfunctions of the linear problem. These functions satisfy general constrains such as regularity at the origin and asymptotic decay at infinity. They are monotonic functions with a single maximum and an arbitrary width. The width and positions of the maximum of the functions are determined to give a maximum growth rate, imposing the constraint that within two growth periods (assuming a ten percent level of turbulence) the growth rate does not change significantly across the peak. Growth rates of two orders of magnitude larger than those given by the standard tearing mode analysis are found.
 Publication:

NASA STI/Recon Technical Report N
 Pub Date:
 January 1994
 Bibcode:
 1994STIN...9622816O
 Keywords:

 Solar Flares;
 Magnetic Field Reconnection;
 Solar Corona;
 Magnetohydrodynamic Waves;
 Magnetohydrodynamic Turbulence;
 Eigenvectors;
 Perturbation;
 Plasma Currents;
 Current Sheets;
 Ohms Law;
 Solar Physics