Field Dynamics on Loss of Relativistic Electrons

Details Field Dynamics on Loss of Relativistic Electrons Field Dynamics on Loss of Relativistic Electrons

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsm34a..03h&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM34A-03

Physics

2730 Magnetosphere: Inner, 2740 Magnetospheric Configuration And Dynamics, 2753 Numerical Modeling, 2774 Radiation Belts

Scientific paper

Trapped relativistic electrons in Earth's magnetosphere respond to the highly dynamic environment in a complex fashion. The dramatic change of field configurations in the inner magnetosphere, especially during magnetic storm time, could significantly alter radiation belt distributions. For example, geosynchronous satellites observe reduced fluxes of relativistic electrons in the dusk sector during geomagnetic storms. Recent studies argued that such flux dropouts are possibly due to the combined effects of stretched dusk-side field lines and inductive electric fields. In this study, we simulate relativistic electron behavior in the inner magnetosphere using the magnetic and electric fields from the Lyon-Fedder-Mobarry global magnetohydrodynamic simulation. The radiation belt model in this work is a two-dimensional test particle simulation which uses the guiding center approximation to describe relativistic electron motion. We drive the MHD simulation with idealized solar wind ram pressure and IMF Bz variations, to quantify the effects of field line stretching and inductive electric fields on the transport and possible loss of outer radiation belt electrons to the magnetopause.

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