Acceleration of Electrons from the Solar Wind to the Inner Magnetosphere During Storms

During magnetic storm recovery, relativistic electron fluxes are usually enhanced over pre-storm values in the inner magnetosphere near geosynchronous orbit. To examine the acceleration of electrons in the inner magnetosphere and the formation of the seed population that provides the source for the relativistic electrons, a study has been undertaken to follow electrons from the solar wind into the magnetosphere during storm events. Electrons are traced in a global MHD model of the solar wind interaction with the Earth's magnetosphere using upstream data both to set the launch parameters of the electrons and to provide the upstream boundary conditions for the MHD simulation. Electron fluxes will be calculated in the inner magnetosphere in the seed region at an equatorial radial distance of 10 Re, and fluxes will also be calculated in the region near geosynchronous orbit. The acceleration of the electrons is affected by inductive electric fields and ULF waves.