A mathematical model of solar flares.
Abstract
The phenomenon of solar flares is modeled assuming that the magnetic field is forcefree and that its evolution is quasistatic. This model is simplified so as to be tractable and yields a semilinear elliptic equation in a halfplane depending on a parameter lambda which describes the time evolution. It is proved that there are (at least) two branches of solutions which have distinct asymptotic behaviors at infinity. The upper branch exists for all lambda greater than 0, but the lower branch exists only on a finite interval /0, lambda exp c/. As stable solutions must have the same asymptotic behavior as the lower branch of solutions, and as this is impossible after lambda exp c, it is contended that no stable solution exists after lambda exp c and that a solar flare is thus triggered.
 Publication:

Quarterly of Applied Mathematics
 Pub Date:
 April 1983
 Bibcode:
 1983QApMa..41....1H
 Keywords:

 Astronomical Models;
 Mathematical Models;
 Solar Flares;
 Branching (Mathematics);
 Elliptic Differential Equations;
 Linear Equations;
 Solar Magnetic Field;
 X Ray Sources;
 Solar Physics;
 Solar Flares:Models