Using Type III Radio Bursts to Track Solar Energetic Particles

Details Using Type III Radio Bursts to Track Solar Energetic Particles Using Type III Radio Bursts to Track Solar Energetic Particles

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh21d..04c&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH21D-04

Physics

7514 Energetic Particles (2114), 7534 Radio Emissions

Scientific paper

Solar electrons are an important component of the flare process. If the electrons gain access to open field lines they produce type III radio emissions at frequencies below 20 MHz. These radio emissions may be used to trace the paths of the causative ( ~10 keV) electrons through the interplanetary medium. Lower and lower frequency emissions correspond to electrons travelling further and further from the Sun until eventually they may reach an observer near 1 AU and produce radio emission locally. Thus given an electron increase at a spacecraft one can trace back the radio emission from low to high frequencies to determine the travel time of the electrons and to validate the flare association. Such a technique suggests that the open field lines from near an active region can extend over some 120° in longitude (and probably in latitude too) in the most energetic events. For flares occurring more than ~60° from the nominal footpoint of an observer's field line the time delays between the flare and the electron arrival time are much longer than the nominal travel time for a distance of ~1.2 AU. The radio data suggest that the delays occur in the interplanetary medium and not at the Sun as is generally assumed. A close association between flares, type III radio bursts and solar particle events in general (i.e. including ions) suggests that the results for the low energy electrons are valid for high energy ions too.

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