Particle Acceleration in the Middle Corona During Relativistic Solar Proton Events of the Current Solar Cycle

Details Particle Acceleration in the Middle Corona During Relativistic Solar Proton Events of the Current Solar Cycle Particle Acceleration in the Middle Corona During Relativistic Solar Proton Events of the Current Solar Cycle

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh42a0772t&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH42A-0772

Physics

2118 Energetic Particles, Solar, 7513 Coronal Mass Ejections, 7514 Energetic Particles (2114), 7519 Flares, 7534 Radio Emissions

Scientific paper

The timing and early temporal evolution of four relativistic solar proton events (GLEs: 6 Nov 1997, 2 May 1998, 14 Jul 2000, 15 Apr 2001) detected by neutron monitors during the current solar cycle are compared with broadband radio observations. These events are accompanied by fast and extended CMEs, as well as flares with widespread signatures of coronal electron acceleration. The related radio sources observed with the Nancay Radio Heliograph cover angular ranges comparable to the CMEs. Besides impulsive acceleration phases, all radio events display time-extended (10 min to several hours) acceleration, at heights between 0.1 and 1 solar radius above the photosphere, well after the maximum of the associated soft X-ray event, and without radiative signatures (X-rays, microwaves) from the low corona and the chromosphere. This shows that energy conversion proceeds in the corona well behind the CME and its presumed shock front. These processes are ignored by models that consider flares as point-like phenomena in space and time. We show that in all four events the onsets of the neutron monitor rises correspond in time to the late radio emission, and argue that the coronal acceleration sites are plausible sources of the relativistic protons detected at 1 AU.

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