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S. J. Bolton, S Levin, M.J. Klein, S Gulkis (JPL), R.M. Thorne (UCLA), J. H. Waite (SWRI), Y Leblanc (CNRS-URA), G. A. Dulk (U. Colorado), R. J. Sault (ATNF)
A model of Jupiter's synchrotron emission will be presented. The model will be compared with recent observations from the Very Large Array (VLA) and the NASA Deep Space Network. Jupiter's synchrotron emission originates from the motion of high energy relativistic electrons trapped in Jupiter's magnetic field and is emitted in an extremely narrow beam in the direction of the electron's motion. This provides the basis for the utilization of the model and remote observations to investigate the electron distribution and magnetic field configuration deep within Jupiter's magnetosphere. We present a progress report on our modeling effort and demonstrate the ability to distinguish various properties regarding the physical characteristics and processes present in Jupiter's radiation belts. (See companion paper, "Changes in the Rotational Beaming Curve of Jupiter's Synchrotron Emission", by Klein et al.).