MAGNETIC STORM MODELING IN THE EARTHS ELECTRON BELT BY THE SALAMMBO CODE

The Salammbo code, which solves the three-dimensional phase-space diff usion equation for the electron radiation belt, was used to explain th e dynamic conditions present during a geomagnetic storm. With a simple injection model, we have characterized the dynamic behavior for relat ivistic electrons in the outer belt. The particles in the range 100 ke V - 500 keV are diffused throughout the belt, with a shape essentially dependent on the radial diffusion coefficients.Particles with higher energies are ''created'' by acceleration of slower particles near the plasmapause location. The calculated shape of the fluxes in an L versu s time grid for the 1 MeV electrons looks globally like those measured aboard the CRRES satellite.