Storm-Dependent Radiation Belt Dynamics

Details Storm-Dependent Radiation Belt Dynamics Storm-Dependent Radiation Belt Dynamics

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm21a0317l&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM21A-0317

Other

2716 Energetic Particles: Precipitating, 2720 Energetic Particles: Trapped, 2730 Magnetosphere: Inner, 2774 Radiation Belts, 2788 Magnetic Storms And Substorms (7954)

Scientific paper

Outer radiation belt electrons have their largest variations during magnetic storms. Taking advantage of recently published phase space density (PSD) data as a function of L* and time, we have developed a comprehensive radial diffusion model, in which both the electron lifetime and source rate are included and parameterized as a function of geomagnetic indices. The PSD data at L*=6 is used as the outer boundary source and the modeled results are directly compared with the PSD data at L*=4. We conclude that the main acceleration mechanism, inward radial diffusion vs in situ acceleration, responsible for the enhancement of outer belt electrons at L*=4 is storm-dependent: in one storm, the enhancement of outer radiation belt electrons can be well explained by inward radial diffusion while in situ acceleration (violating the first adiabatic invariant) has to be invoked to explain the enhancement of the outer belt electrons during another storm.

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