Electron Transport in the Earth's Outer and Inner Magnetosphere

Details Electron Transport in the Earth's Outer and Inner Magnetosphere Electron Transport in the Earth's Outer and Inner Magnetosphere

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsm33b..06s&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SM33B-06

Physics

2720 Energetic Particles, Trapped, 2730 Magnetosphere: Inner, 2731 Magnetosphere: Outer, 2753 Numerical Modeling

Scientific paper

As electrons are transported from the solar wind and through the Earth's magnetosphere, they can be accelerated to energies > 10 keV when they reach the so-called seed region located at about 10 RE radially from the Earth in the equatorial plane. As these seed electrons move closer to the Earth, wave-particle interactions can cause further acceleration of electrons to relativistic (MeV) energies. This process occurs during the recovery of magnetic storms, where relativistic electron fluxes are usually observed to be enhanced over pre-storm values in the inner magnetosphere near geosynchronous orbit. In this study, the transport of electrons from the solar wind and outer magnetosphere towards the seed region is examined. This is done by following electron trajectories from different starting points in a global model for the magnetospheric magnetic and electric fields. The electron particle trajectories are followed based on the guiding center approximation and both an empirical and an MHD model (BATS-R-US code) are used for the global magnetospheric fields. In regions where the local fields are very weak (e.g., near reconnection regions), non-adiabatic effects could be important and this is included when following electrons by switching from the guiding center approximation to a full trajectory calculation using the Lorentz force equation in these localized regions of space. Electron distribution functions formed at different locations in the magnetotail as well as in the seed region will be discussed.

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