Backstreaming Electrons Associated With Solar Electron Bursts

Details Backstreaming Electrons Associated With Solar Electron Bursts Backstreaming Electrons Associated With Solar Electron Bursts

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh44c..02s&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH44C-02

Physics

2100 Interplanetary Physics, 2114 Energetic Particles (7514), 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma

Scientific paper

Solar electron bursts are frequently observed in the ACE/SWEPAM suprathermal electron measurements at energies below 1.4 keV. A significant fraction of such events show backscattered electrons, beginning after the burst onset and traveling back towards the Sun along the magnetic field direction. Such backscattered particles imply a scattering mechanism beyond the spacecraft location. Some bursts also show backstreaming conic distributions, implying mirroring at magnetic field enhancements beyond the spacecraft. Here we present a study of these backstreaming particles during solar electron events. We examine the occurrence of backstreaming electrons and their relationship to other burst characteristics such as pitch angle width, duration, and energy range. We also investigate the time delay between burst onset and the appearance of backscattered electrons, including energy and pitch-angle dispersion. We examine the pitch angle distribution and energy dependence of backstreaming electrons, and consider possible origins of these electron distributions and their relationship to solar wind structure beyond the spacecraft.

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