Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh31c..09k&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SH31C-09
Physics
2118 Energetic Particles, Solar, 7513 Coronal Mass Ejections, 7514 Energetic Particles (2114), 7519 Flares, 7534 Radio Emissions
Scientific paper
The large solar particle event of 6 November 1997 produced energetic electrons and protons up to relativistic energies observed at 1 AU. Solar phenomena comprised an intense flare, a rapid CME and a propagating disturbance seen at EUV ('EIT-wave'). Following widespread practice, the particle signatures detected in space have been discussed in the literature in terms of acceleration by the shock driven by the CME. Coronal processes closer to the flaring active region were mostly disregarded, although high Fe charge states measured at tens of MeV seem to suggest acceleration in a relatively dense plasma. While hard and soft X-ray and microwave signatures of the flare show a rather impulsive event with duration between ten and a few tens of minutes, spectra and images at decimetric and longer waves reveal that electrons are accelerated in the corona during more than an hour after the start of the flare. The spectral characteristics of these emissions suggest that the thermal electron densities in the source region range from some 108 to a few 109 cm-3. The radio maps show stable sources above the active region, while the front of the CME and the shock revealed by type~II radio emission were at several solar radii above the photosphere. We discuss the timing and spectral characteristics of the coronal radio emissions, compare them with reported properties of particles at 1 AU, and suggest that the coronal acceleration supplies part of these particles.
Klein Karsten
Trottet Gerard
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