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Title:
A flare model deduced from HINOTORI and millimeterwave interferometer observations
Authors:
Kawabata, K.-A.; Ogawa, H.; Suzuki, I.
Affiliation:
AC(Nagoya University, Nagoya, Japan)
Journal:
(Japan Society for the Promotion of Science and National Science Foundation, U.S.-Japan Seminar on the Recent Advances in the Understanding of Solar Flares, Tokyo, Japan, Oct. 5-8, 1982) Solar Physics (ISSN 0038-0938), vol. 86, July 1983, p. 247-251; Discussion, p. 251, 252. (SoPh Homepage)
Publication Date:
07/1983
Category:
Solar Physics
Origin:
STI
NASA/STI Keywords:
SOLAR FLARES, SOLAR RADIO EMISSION, SOLAR X-RAYS, ELECTRON ACCELERATION, GAMMA RAY SPECTRA, HIGH ENERGY ELECTRONS, HIGH TEMPERATURE PLASMAS, MILLIMETER WAVES, SOLAR ELECTRONS, SUNLIGHT
Bibliographic Code:
1983SoPh...86..247K

Abstract

The spatial distributions of energetic electrons and high-temperature plasma are investigated using data from the gamma-ray and white-light flare of 13 May 1981. It is found that the electron density of the ambient plasma was 3 x 10 to the 10th/cu cm, at which density the ionization loss times of 20 keV, 100 keV, 300 deV, and 4 MeV electrons become 0.5, 5, 30, and 350 seconds, respectively. It is determined that electrons below 30 keV are not able to escape from the source region. Radio observations at 35 GHz indicate that electrons with an energy of several MeV are trapped in the source. It is suggested that the radio brightness at the sunspot may be due to the precipitation of electrons in the loss-cone, and that the time history of radio brightness may be a manifestation of the rate of particle acceleration. The time delay of 3 minutes observed at hard X-ray and gamma-ray energies and in the 35 GHz flux density indicates that it takes 3 minutes to accelerate electrons up to 300 keV.

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