Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm21a0333k&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SM21A-0333
Physics
2720 Energetic Particles: Trapped, 2753 Numerical Modeling, 2774 Radiation Belts
Scientific paper
It has been suggested that drift loss to the magnetopause can be one of the major loss mechanisms contributing to the relativistic electron flux dropout. In this study, we examine details of relativistic electrons' drift physics to determine the extent to which the drift loss through the magnetopause is important to the total loss of the outer radiation belt. We have numerically computed drift paths of relativistic electrons' guiding center for various pitch angles, various positions and different solar wind conditions using Tsyganenko T02 model. We specifically demonstrate how the drift loss effect depends on these various parameters. It is shown that the drift loss effect is more likely expected for a higher pitch angle and near midnight and then spreads to lower pitch angles and dusk and dawn MLT regions as the dynamic pressure increases or IMF BZ becomes more southward. Most importantly, we present various estimates of relative changes of omni-directional flux of 1MeV electrons between two different solar wind conditions based on a simple form of the directional flux function. For a change of the dynamic pressure from 4 nPa to 10 nPa with a fixed IMF BZ=0 nT, our estimate indicates that the omni- directional flux for the 10 nPa pressure at the equator at midnight near geosynchronous altitude decreases by ~56 to 97%, depending on a specific pitch angle dependence of the directional flux function, compared to that for the 4 nPa pressure. The effect is somewhat lower at pre- and post-midnight MLTs, and rapidly declines at inner regions than geosynchronous orbit. It however becomes more substantial at measurement positions away from the equator. A qualitatively similar, but quantitatively different, result has been obtained for two different conditions of IMF BZ.
Choi Changsu
Kim Hungsoo
Kim Kyounghee
Lee Daehee
Lee Edward
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