Type III radio burst productivity of solar flares. I - Release of energetic electrons out of the flare site

Details Type III radio burst productivity of solar flares. I - Release of energetic electrons out of the flare site Type III radio burst productivity of solar flares. I - Release of energetic electrons out of the flare site

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..130..101p&link_type=abstract

(Committee of European Radio Astronomers, SNSF, URSI, et al., Workshop on Particle Beams in the Solar Atmosphere, Braunwald, Swi

Physics

6

Electron Beams, H Alpha Line, Solar Flares, Type 3 Bursts, Astronomical Spectroscopy, Interplanetary Medium, Predictions, Spatial Distribution, Stellar Mass Ejection

Scientific paper

The statistical relationship between type III radio bursts and optical flares, using the comprehensive flare data base at the NOAA National Geophysical Data Center (Boulder, Colorado), and the radio observations obtained with the ARTEMIS multichannel spectrograph in Nancay (France), operating at 500-100 MHz are presented. At variance with previous results, it is seen that type III probability of occurrence depends only weakly upon the spatial extension of the flare observed in H-alpha, but strongly upon its brightness. It is confirmed that the type III probability increases with proximity to sunspots and with mass motions (surges and prominence activity); in addition, statistical data are consistent with both relations holding at fixed flare brightness. Thus, some of the conditions favorable to type III occurrence are characteristic of compact flares, while others are characteristic of large and long-duration flares, which are often related to mass ejections. This apparent paradox suggests that particle acceleration and magnetic expansion are at work simultaneously in the ejection of electron streams out of faring sites.

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