Two types of ion energy dispersions observed in the nightside auroral regions during geomagnetically disturbed periods

Details Two types of ion energy dispersions observed in the nightside auroral regions during geomagnetically disturbed periods Two types of ion energy dispersions observed in the nightside auroral regions during geomagnetically disturbed periods

Apr 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996jgr...101.7749h&link_type=abstract

Journal of Geophysical Research, Volume 101, Issue A4, p. 7749-7768

Physics

Plasma Physics

24

Magnetospheric Physics: Magnetospheric Configuration And Dynamics, Ionosphere: Particle Precipitation, Magnetospheric Physics: Storms And Substorms, Space Plasma Physics: Charged Particle Motion And Acceleration

Scientific paper

The Akebono satellite has observed two types of energy dispersion signatures of discrete ion precipitation event in the nightside auroral regions during active geomagnetic conditions. The charged particle experiments and electric and magnetic field detectors on board Akebono provide us with essential clues to characterize the source regions and acceleration and/or injection processes associated with these two types of ion signatures. The magnetic field data obtained simultaneously by the geosynchronous GOES 6 and 7 satellites and the ground magnetograms are useful to examine their relationships with geomagnetic activity. Mass composition data and pitch angle distributions show that different sources and processes should be attributed to two types (Types I and II) of energy dispersion phenomena. Type I consists of multiple bouncing ion clusters constituted by H+. These H+ clusters tend to be detected at the expansion phase of substorms and have characteristic multiple energy-dispersed signatures. Type II consists of O+ energy dispersion(s), which is often observed at the recovery phase. It is reasonable to consider that the H+ clusters of Type I are accelerated by dipolarization at the equator, are injected in the field-aligned direction, and bounce on closed field lines after the substorm onset. We interpret these multiple energy dispersion events as mainly due to the time-of-flight (TOF) effect, although the convection may influence the energy-dispersed traces. Based of the TOF model, we estimate the source distance to be 20-30 RE along the field lines. On the other hand, the O+ energy dispersion of Type II is a consequence of reprecipitation of terrestrial ions ejected as an upward flowing ion (UFI) beam from the upper ionosphere by a parallel electrostatic potential difference. The O+ energy dispersion is induced by the E×B drift during the field-aligned transport from the source region to the observation point.

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