Application of The Alfvén-Assisted Precipitation Model to Field-Aligned Electron Bursts

Details Application of The Alfvén-Assisted Precipitation Model to Field-Aligned Electron Bursts Application of The Alfvén-Assisted Precipitation Model to Field-Aligned Electron Bursts

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsa23a1464l&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SA23A-1464

Computer Science

Sound

[2407] Ionosphere / Auroral Ionosphere, [2431] Ionosphere / Ionosphere/Magnetosphere Interactions, [2455] Ionosphere / Particle Precipitation, [2483] Ionosphere / Wave/Particle Interactions

Scientific paper

A close relationship between field-aligned electron bursts and Alfvén waves has been identified by numerous sounding rocket and satellite missions. While previous work has demonstrated the ability of inertial Alfvén waves to accelerate electrons along the geomagnetic field lines in the dayside cusp, the nightside signatures of Alfvén wave interactions with cold electrons in the auroral ionosphere have yet to be explained in a reasonable manner. The Alfvén-assisted precipitation model and new analyses of observations supporting its validity are presented. High time resolution electron flux data from the GEODESIC sounding rocket flight of 2000, taken during an active auroral breakup, show dozens of field-aligned electron bursts; the bursts display energy-time dispersion with higher energy electrons appearing earlier in time and have peak energies with a range up to—but not exceeding—the energy of a nearby inverted-V peak, up to about 20 keV. Several of these bursts occur separately from inverted-V electron distributions and an instance of a burst occurring near the edge of an auroral arc with fluxes higher than the accompanying inverted-V electron distribution is also present. The observations not only suggest separate source locations for the burst electrons and the quasistatic, isotropic inverted-V electrons, but also support the existence of a quasistatic potential structure without simultaneous inverted-V electron precipitation. The model incorporates the aforementioned attributes displayed by the observations and provides a set of physical parameters which help characterize individual phenomena. Energy-time dispersion signatures are derived and shown for each of the individual bursts; model fits to these signatures demonstrate agreement with the model. Examples from Freja and FAST satellite data are also discussed.

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