Solar Origin of Interplanetary Impulsive Electron Events

Details Solar Origin of Interplanetary Impulsive Electron Events Solar Origin of Interplanetary Impulsive Electron Events

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh22a..03p&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH22A-03

Physics

2114 Energetic Particles, Heliospheric (7514), 2118 Energetic Particles, Solar

Scientific paper

Many solar impulsive electron events have been traditionally associated with type III radio emissions. Several recent studies however showed that, in the majority of the events, the solar release of electrons at high energies can present delays of up-to-half an hour with respect of the onset of type III bursts. We have revisited the origin of a large number of events using multiwave-length observations. For each event, we investigated the coronal restructuring using EUV, white-light, radio imaging and spectral observations in a wide frequency range that allows us to follow the evolution of the corona from a few tenths above the solar limb up to a few solar radii. Radio observations revealed direct energetic electron signatures, close in time with the electron release. The release time for the delayed events always coincides with the onset or major changes in the complex of radio emissions. This close association indicates that the coronal processes involved in the radio emissions are at the origin of the electron acceleration. We illustrate our results by presenting, more particularly, one recent event for which the observations were also coupled with imaging spectroscopy measurements obtained by the RHESSI mission (from 3 keV to 17 MeV). RHESSI observed a hard X-ray emission, which lasted for more than fifteen minutes. This emission was closely associated in time and space with the radio emission imaged by the Nançay Radioheliograph. The results suggest that, for this event, both electrons detected in the corona and those injected in the interplanetary medium are due to a similar process involving coronal magnetic field interactions. Their respective sites of acceleration/injection are however distinct in space and time. The energetic electrons detected in the interplanetary medium are not released during the X-ray burst.

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