Proton Aurora and Trapped Particle Substorm Dynamics Compared

Details Proton Aurora and Trapped Particle Substorm Dynamics Compared Proton Aurora and Trapped Particle Substorm Dynamics Compared

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsm32b..05j&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SM32B-05

Physics

2704 Auroral Phenomena (2407), 2720 Energetic Particles, Trapped, 2730 Magnetosphere: Inner, 2764 Plasma Sheet, 2788 Storms And Substorms

Scientific paper

Global auroral imaging data have shown us that auroral substorms are highly dynamic, complex and structured events. Since they are the result of processes taking place along extended magnetic field lines, auroral displays have been called the "TV screen" for the magnetoshpere. With recent IMAGE energetic neutral atom (ENA) observations we can globally correlate the dynamics of precipitating proton auroral phenomena with the dynamics of non-precipitating ENA substorm phenomena, tying processes in different regions along magnetic field lines together. We present comparisons for FUV proton aurora and MENA medium energy ENA observations of isolated substorm events during the summer of 2001. Both techniques show expected increases of particle fluxes during the expansion phase. The proton auroral response is typically quicker and initially stronger, with significant flux increases over short periods of time. The ENA response is more gradual, but enhanced flux levels will also persist up to several hours, much longer than the by comparison short-lived auroral displays. While this represents a considerable difference, the local time extent of auroral and ENA particles tracks much more closely. We will focus on this latter aspect of comparing the geophysical "topography" of trapped and precipitating particles.

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