Backscattering of solar electron burst distributions

Details Backscattering of solar electron burst distributions Backscattering of solar electron burst distributions

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh24a..07s&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH24A-07

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. Approximately 1/3 of such events show backstreaming electrons, which are typically observed after a 1-2 hour delay following burst onset and travel back towards the Sun along the magnetic field direction. These backstreaming particles are likely produced by scattering of the solar electron burst particles beyond the ~1 AU spacecraft location. Our previous studies have shown that transient solar burst electrons exhibit a greater degree of pitch angle scattering than does the steady-state solar wind electron strahl, which could result in turning back of the burst electrons. From the delays observed between the onset of the bursts and the backstreaming, we infer that burst electrons are turned back sunward at a field-aligned distance of less than 1 AU beyond the spacecraft. In this study we compare the fluxes and energy spectra of backstreaming particles with those of the outgoing burst particles. In addition, we compare the angular widths of the two electron beams. These comparisons provide an indication of the relative importance of magnetic mirroring and focusing, scattering in pitch angle, and scattering in energy for determining the character of the observed electron distributions.

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