Scatter-free impulsive electron event from the October 28, 2003 X17 flare

Details Scatter-free impulsive electron event from the October 28, 2003 X17 flare Scatter-free impulsive electron event from the October 28, 2003 X17 flare

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh51a..10k&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH51A-10

Physics

7514 Energetic Particles (2114), 7534 Radio Emissions, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

The October 28, 11 UT X-17 flare produced an impulsive electron event detected near the Earth by the WIND 3D Plasma & Energetic Particles instrument from ~200 keV down to ~1~keV, even though the flare was located around E08 and therefore unlikely to be magnetically connected to Earth. This impulsive event exhibited a fast rise and decay (~10 min each), and was followed by a second, much slower rising event that lasted for many hours. The peak times of the impulsive event show clear velocity dispersion consistent with a path length of 1.27±0.1 AU, indicating that the electron propagation is essentially scatter-free. Onset time analysis reveal that the impulsive event electrons left the Sun at 11:14±3 UT, just after the end of a group of type III bursts seen at 14~MHz (11:03-11:11~UT) and when the type II burst reaches 14~MHz. Radio pulsations at 0.6-1.3~GHz were seen between 11:14:30 and 11:22:00~UT. The velocity dispersion seen in the peak times suggests that the peak of the injection occurred around 11:25±3~UT roughly consistent with the end of the decimeter radio emission. This impulsive electron event also was observed near Mars at energies from ~1 to 20~keV by the Electron Reflectometer instrument on Mars Global Surveyor spacecraft.

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