Dispersed ion structures at the poleward edge of the auroral oval: Low-altitude observations and numerical modeling

Details Dispersed ion structures at the poleward edge of the auroral oval: Low-altitude observations and numerical modeling Dispersed ion structures at the poleward edge of the auroral oval: Low-altitude observations and numerical modeling

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....9819181b&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. A11, p. 19,181-19,204

Physics

39

Auroral Zones, Boundary Layer Plasmas, Dispersion, Geomagnetic Tail, Geomagnetism, Ion Beams, Mathematical Models, Particle Precipitation, Polar Substorms, Auroral Electrojets, Earth Magnetosphere, Magnetic Field Configurations, Magnetic Mirrors, Particle Acceleration, Solar Terrestrial Interactions, Solar Wind, Statistical Analysis

Scientific paper

We have compared the AUREOL 3 (A3) observations of auroral ion precipitation, particularly ion beams, with the results from the global kinetic model of magnetotail plasma of Ashour-Abdalla et al. (1993). We have identified 101 energetic keV H(+) velocity dispersed precipitating ion structures (VDIS) with fluxes above 10-3 ergs./sq cm./s in the A3 record between the end of 1981 and mid-1984. These beams display a systematic increase in energy with increasing latitude and were observed in a narrow region within less than 1 deg in latitude of the polar cap boundary. The VDIS are the most distinctive feature in the auroral zone of the plasma sheet boundary layer. We report first on a statistical analysis of the possible relationships between magnetic activity or substorm phase and the VDIS properties. Our particle simulations of the precipitating ions have been extended by using a series of modified versions of the Tsyganenko (1989) magnetic field model and by varying the cross-magnetosphere electric field. In the simulations, plasma from a mantle source is subject to strong nonlinear acceleration, forming beams which flow along the PSBL. Only 3 to 4% of these beams precipitate into the ionosphere to form the VDIS while the majority return to the equatorial plane after mirroring and form the thermalized central plasma sheet. The final energy and the dispersion of the beams in the model depend on the amplitude of the cross-tail electric field. Two unsual observations of low-energy (less than 5 keV) O(+) VDIS, shifted by 4 deg 5 deg in invariant latitude equatorward of H(+) VDIS are analyzed in detail. The sparsity of such O(+) events and the absence of the changes in the flux and frequency of occurrence indicate a solar wind origin for the plasma. Finally, large-scale kinetic modeling, even with its simplifications and assumptions (e.g., static magnetic field, solar wind source), reproduces low-altitude auroral ion features fairly well; it may therefore be presented as an appropriate framework into which data on energization and transport of the hot plasma, obtained in the equatorial plane, could be inserted in the near future.

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