Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm54a..05z&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SM54A-05
Physics
0310 Airglow And Aurora, 2455 Particle Precipitation, 2475 Polar Cap Ionosphere, 2704 Auroral Phenomena (2407), 2784 Solar Wind/Magnetosphere Interactions
Scientific paper
The energy flux of polar rain, the precipitating electrons directly from the solar wind, is usually too weak to create observable auroral emissions. However, intense polar rain with mean energy above 1 keV was observed at times by in situ electron spectrometers. The energy flux of the intense keV polar rain is great enough that it can excite detectable optical aurora: we term this the polar rain aurora. Observations of polar rain aurora will help to reveal some new features on solar wind electron entry into the polar cap. Global FUV auroral imagers observed, for the first time, a few polar rain aurora events. In this paper we will present observations and interpretation of the structures (such as dawn-dusk alignment, etc) and anti-sunward motion of polar rain auroras and their associated solar wind and IMF conditions. Possible mechanisms for the observed features will also be discussed.
Paxton Larry J.
Zhang Yajing
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