The Jovian Synchrotron Emission's Time Variability and the Radiation-Belt Electrons Dynamics

Details The Jovian Synchrotron Emission's Time Variability and the Radiation-Belt Electrons Dynamics The Jovian Synchrotron Emission's Time Variability and the Radiation-Belt Electrons Dynamics

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsm33c0471s&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SM33C-0471

Physics

2774 Radiation Belts

Scientific paper

The time variability of the synchrotron emission in Jupiter's inner magnetosphere provides a unique opportunity to enhance our understanding of the origins and dynamics of the radiation-belt electrons. Based on a theoretical approach (physical modeling of the Jovian electron radiation belts), analysis of in-situ data in the vicinity of Jupiter and Earth (Galileo orbiter data during its full tour, Pioneer and Voyager 2 measurements, WIND data), and radio data (VLA and DNS observations), we will discuss the dependence of the Jovian synchrotron emission (10h and long-term fluctuations, radio spectrum) on physical parameters capable of driving the activity of the high-energy electrons in Jupiter's magnetosphere. The results of our work confirm the control of Jupiter's synchrotron emission by the solar wind. The results show a strong correlation between the radio emission, the radiation-belt electron transport and the solar wind RAM pressure. Radial diffusion and particle injection in the inner magnetosphere appear to respond to the solar wind pressure with different time scales and give an explanation for the observed long-term variation in the synchrotron emission.

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