A comparison of gamma-ray and radio emissions during the 11:42 UT solar flare on 1982 June 3

Details A comparison of gamma-ray and radio emissions during the 11:42 UT solar flare on 1982 June 3 A comparison of gamma-ray and radio emissions during the 11:42 UT solar flare on 1982 June 3

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...288..647t&link_type=abstract

Astronomy and Astrophysics 288, 647-655 (1994)

Astronomy and Astrophysics

Astrophysics

25

Acceleration Of Particles, Sun: Activity, Flares, Radio Radiation, Gamma Rays

Scientific paper

We report new, unpublished data for the X class solar flare on 1982 June 3 at 1142 UT (X8), using data from the SMM GRS, the Nancay Radioheliograph, the RSTN network, and two optical observatories. We demonstrate that ion and relativistic electron acceleration both occur before the rise of the initial major photon burst. We have also carried out a detailed comparison of the time histories for emissions at 169 MHz, several microwave frequencies, and X-ray and γ-ray energies from 14 keV to above 10 MeV. The comparisons clearly show: (i) a close time correlation of all emissions during the initial phase of the event, indicating that acceleration (or release) of the electrons and ions responsible for the different emissions likely came from the same source, (ii) the different hard X-ray and γ ray peaks are associated with the appearance of new 169 MHz radio sources. During the later phase of this event the energetic emissions were predominately γ rays and high-energy neutrons resulting from an extended acceleration or trapping plus precipitation phase characterized by energetic ions with energies up to a GeV with little or no evidence for the presence of relativistic electrons. During this time a moving Type IV burst developed and persisted for at least 6 minutes. The Nancay radioheliograph data do not show evidence for a large scale coronal Type II shock. The results presented here show that the magnetic field topology of the acceleration region evolves throughout the event indicating that acceleration in proposed simple single loop models is not viable. From this analysis we conclude that the two bursts of high-energy emissions which characterize this flare are due to two different particle populations, which are accelerated and propagate in different magnetic structures.

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