Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm21b..01h&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SM21B-01
Physics
[2772] Magnetospheric Physics / Plasma Waves And Instabilities, [2774] Magnetospheric Physics / Radiation Belts, [2788] Magnetospheric Physics / Magnetic Storms And Substorms
Scientific paper
The relativistic electron flux in the outer radiation belt can vary by up to five orders of magnitude during geomagnetic disturbances driven by the solar wind. These variations are hazardous to spacecraft and humans and affect the chemistry and dynamics of the upper atmosphere. Understanding what causes variations in the radiation belts and how they are related to changes in the solar driver are challenging problems requiring a coordinated theory, modelling, and data analysis effort. Recent research has identified some of the key physical processes and has simulated the development of dynamic global radiation belt models to test ideas in preparation for new missions such as RBSP, and which may have other space weather applications. In this overview we describe some of the key physical processes, including radial diffusion, loss and acceleration due to wave-particle interactions, and how they depend on changes in the source population and plasma boundaries. We describe some of the recent attempts to incorporate these processes into global models, some of the differences between the models, and how well the results compare with data. Finally we comment on some of the issues that need to be addressed in future, and the potential for applying these models to space weather.
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