Phase Space Distribution of Relativistic Electrons near Geosynchronous Orbit in Storm Times

Details Phase Space Distribution of Relativistic Electrons near Geosynchronous Orbit in Storm Times Phase Space Distribution of Relativistic Electrons near Geosynchronous Orbit in Storm Times

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsm41a..09c&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SM41A-09

Physics

2700 Magnetospheric Physics, 2720 Energetic Particles, Trapped, 2740 Magnetospheric Configuration And Dynamics, 2756 Planetary Magnetospheres (5443, 5737, 6030), 2788 Storms And Substorms

Scientific paper

Understanding the behavior of relativistic electrons in the Earth's radiation belts in geomagnetic storms is of keen interest to the space physicists' community due to both theoretical and practical concerns. After decades of efforts to describe the relativistic electrons dynamics in storm times, currently existing models succeed in either fitting parts of the observations or in simulating one storm only. The differentiation of competing theories calls for a data-assimilation based global electron phase space density model. Since the calculation of phase space density greatly relies on the accuracy of the storm magnetospheric field, a new approach is established to choose the best model by comparing with the multiple measurements from GOES and POLAR satellites. Then the output from the model is optimized by fine-tuning input parameters in a time-dependent fashion, to obtain the best fit dynamic model. The choice of the magnetic field model is also tested by Liouville's theorem, which requires the conserved phase space density for the fixed phase space coordinates. The calculation of phase space density is based on the choice of the storm-time magnetic field model and, as the first step of the global model development, data from LANL geosynchronous SOPA instruments. By employing a technique developed previously, we can deduce the electron phase space density distribution for the region around geosynchronous orbit, covering a range of L*~6-7, which also establishes the radial PSD gradient as a function of both universal time, local time in storm-time.

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