A COMPARISON OF GAMMA-RAY AND RADIO EMISSIONS DURING THE 11 42 UT SOLAR-FLARE ON 1982 JUNE 3/

We report new, unpublished data for the X class solar flare on 1982 Ju ne 3 at 1142 UT (X8), using data from the SMM GRS, the Nancay Radiohel iograph, the RSTN network, and two optical observatories. We demonstra te that ion and relativistic electron acceleration both occur before t he rise of the initial major photon burst. We have also carried out a detailed comparison of the time histories for emissions at 169 MHz, se veral microwave frequencies, and X-ray and gamma-ray energies from 14 keV to above 10 MeV. The comparisons clearly show: (i) a close time co rrelation of all emissions during the initial phase of the event, indi cating that acceleration (or release) of the electrons and ions respon sible for the different emissions likely came from the same source, (i i) the different hard X-ray and gamma ray peaks are associated with th e appearance of new 169 MHz radio sources. During the later phase of t his event the energetic emissions were predominately gamma rays and hi gh-energy neutrons resulting from an extended acceleration or trapping plus precipitation phase characterized by energetic ions with energie s up to a GeV with little or no evidence for the presence of relativis tic electrons. During this time a moving Type IV burst developed and p ersisted for at least 6 minutes. The Nancay radioheliograph data do no t show evidence for a large scale coronal Type II shock. The results p resented here show that the magnetic field topology of the acceleratio n region evolves throughout the event indicating that acceleration in proposed simple single loop models is not viable. From this analysis w e conclude that the two bursts of high-energy emissions which characte rize this flare are due to two different particle populations, which a re accelerated and propagate in different magnetic structures.