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Solar filament eruptions and energetic particle events
Kahler, S. W.; Cliver, E. W.; Cane, H. V.; McGuire, R. E.; Stone, R. G.; Sheeley, N. R., Jr.
AA(Emmanuel College, Boston, MA), AB(USAF, Geophysics Laboratory, Bedford, MA), AC(NASA, Goddard Space Flight Center, Greenbelt, MD), AD(NASA, Goddard Space Flight Center, Greenbelt, MD), AE(NASA, Goddard Space Flight Center, Greenbelt, MD)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 302, March 1, 1986, p. 504-510. (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Energetic Particles, Particle Acceleration, Solar Corona, Solar Flares, Solar Prominences, Energy Spectra, H Alpha Line, Shock Waves, Solar X-Rays
Bibliographic Code:


The 1981 December 5 solar filament eruption that is associated with an energetic (E greater than 50 MeV) particle event observed at 1 AU. The eruption was photographed in H-alpha and was observed by the Solwind whitelight coronagraph on P78-1. It occurred well away from any solar active region and was not associated with an impulsive microwave burst, indicating that magnetic complexity and a detectable impulsive phase are not required for the production of a solar energetic particle (SEP) event. No metric type II or IV emission was observed, but an associated interplanetary type II burst was detected by the low-frequency radio experiment on ISEE 3. The December 5 and two other SEP events lacking evidence for low coronal shocks had unusually steep energy spectra (gamma greater than 3.5). In terms of shock acceleration, this suggests that shocks formed relatively high in the corona may produce steeper energy spectra than those formed at lower altitudes. It is noted that the filament itself maybe one source of the ions accelerated to high energies, since it is the only plausible coronal source of the He(+) ions observed in SEP events.

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