How the Plasmapause Affects Relativistic Electron Variability in the Outer Radiation Belt

Details How the Plasmapause Affects Relativistic Electron Variability in the Outer Radiation Belt How the Plasmapause Affects Relativistic Electron Variability in the Outer Radiation Belt

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsm31a..02t&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SM31A-02

Physics

2716 Energetic Particles, Precipitating, 2720 Energetic Particles, Trapped, 2730 Magnetosphere: Inner, 2768 Plasmasphere, 2772 Plasma Waves And Instabilities

Scientific paper

Variability of energetic electrons in the outer radiation belt is due to an imbalance between source and loss processes. Source processes include radial diffusion (driven by enhanced ULF waves) and local stochastic acceleration by VLF plasma waves, while losses are primarily due to wave-particle scattering and ultimate loss to the atmosphere. At the onset of a magnetic storm, despite a pronounced increase in the source of acceleration, losses usually dominate causing a net depletion of relativistic outer zone flux. Flux increases can occur during the storm recovery, when losses become less pronounced. The plasmapause location plays a fundamental role in controlling the effectiveness of the source and loss processes. Enhanced ULF waves and VLF chorus emissions are primarily excited outside the plasmapause during disturbed conditions. Both waves contribute to the acceleration source. Intense EMIC waves, excited along the dusk-side plasmapause (and plume) can provide an effective scattering loss for relativistic electrons, especially during the main phase of a storm as ring current protons are injected into the system. Recent theoretical simulations of the effectiveness of potential source and loss processes will be presented, and related to the location of the disturbed plasmapause location.

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