Other
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm52a..06m&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SM52A-06
Other
2720 Energetic Particles, Trapped, 2730 Magnetosphere: Inner, 2788 Storms And Substorms
Scientific paper
Since the discovery of the radiation belts in the late 1950's, many observations and theoretical studies on their time variations have been carried out. As for the long term variation (e.g., solar cycle), however, there are few studies, and it has not been well understood. This is because of the limited long term homogeneous data set of the radiation belt particles expect for the geosynchronous orbit. In this study, we have performed analysis to investigate the energy and spatial dependence of the solar cycle variation on energetic electrons in the whole radiation belts, using the data set from the TIROS/NOAA satellites during the period from 1979 to 1999. The existence of variation synchronized with the solar cycle in both the inner and outer radiation belts was confirmed. The relativistic electron (> 300 keV) flux, at the region of L < 4, enhanced after the solar maximum and was absent near the solar minimum. The rise time of the flux increase was shorter than the flux decrease. On the contrary, at the region of L > 5, the electron flux was absent in solar maximum, and the flux increased near the solar minimum. The rise time of the flux increase was longer than the flux decrease. This phase difference between the region of L < 4 and L > 5 was shorter compared with the diffusion time expected from the traditional radial diffusion coefficients. \The flux peak of outer belt relativistic electrons shifted inward during the solar maximum, while shifted outward during the solar minimum. It was also shown that the peak position moved concurrently with the plasmapause location. This global motion of the outer belt suggested the possibility that thermal plasma distribution and/or convection electric field were control parameter of generation/dissipation of relativistic electrons. These results cannot be explained by the traditional radial diffusion process alone, and suggest the fast radial diffusion or another transport/acceleration process inside the radiation belts.
Misawa Hiroaki
Miyoshi Yasunobu
Morioka Akira
Obara Takahiro
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