Connecting Dusk-side Relativistic Electron Precipitation and Equatorial Electron Flux

Details Connecting Dusk-side Relativistic Electron Precipitation and Equatorial Electron Flux Connecting Dusk-side Relativistic Electron Precipitation and Equatorial Electron Flux

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsm43b1502s&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SM43B-1502

Physics

2716 Energetic Particles: Precipitating, 2720 Energetic Particles: Trapped, 2774 Radiation Belts

Scientific paper

The significant variability in the measured flux of relativistic (~MeV) electrons in the Earth's outer radiation belt is the result of competing acceleration and loss processes. Several distinct loss processes have been identified which individually can significantly and rapidly (~1 day) deplete the radiation belt. Precipitation of electrons in the atmosphere by resonant wave-particle interactions is one such loss process. Different modes of such atmospheric loss should be distinguishable by their dependence on L-shell and local time. This poster will connect direct observations of loss made by the MINIS balloon campaign during commencement of the January 21, 2005 magnetic storm to observations of the pre- and post-storm fluxes made by several GPS satellites. MINIS observed bremsstrahlung X-rays produced by relativistic electron precipitation from the outer radiation belt. At the time there were two MINIS balloons located in the dusk sector near L=4 where GPS makes an equatorial crossing. We will present results showing the scattering efficiency as a function of energy, relative flux in the local loss cone, and total observed loss rate. We also place limits on the spatial scale of the precipitation by comparing the observed loss rate to the net change in trapped flux.

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