Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992egre.symp.....k&link_type=abstract
In Max-Planck-Inst. für Physik und Astrophysik, EGRET Mission and Data Analysis 5 p (SEE N94-19462 04-89)
Astronomy and Astrophysics
Astrophysics
Bremsstrahlung, Gamma Ray Spectrometers, Light Curve, Solar Flares, Spectrum Analysis, Compton Effect, Gamma Ray Observatory, Gamma Ray Telescopes, Light (Visible Radiation), Light Emission, Solar Spectrometers
Scientific paper
On 11 Jun. 1991, the Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory (Comption-GRO) observed high energy gamma radiation above 30 MeV from the Sun following an intense flare around 2:00 Universal Time (UT). After the decay of most of the x ray flare, which caused nearly complete deadtime losses in EGRET, high energy emission was registered during the interval from about 3:30 UT to at least 10:30 UT. Gamma rays were detected up to energies above 1 GeV. The solar origin of the emission is assured by the time profile of the gamma ray count rate and by time resolved sky maps, which show a clear maximum at the position of the sun. The gamma ray lightcurve of the flare can be described with two components: a fast decaying emission with an e-folding time constant of about 25 minutes and a slow decay with about 255 minutes. There are indications for a spectral evolution with time, such that the emission below 100 MeV fades away earlier than the 100 to 300 MeV radiation, roughly in the time scale of the fast component. The spectrum of the flare can be fitted with a composite of a proton generated pion neutral spectrum and an electron bremsstrahlung component. The latter can be identified with the fast decaying component of the lightcurve.
Bertsch David L.
Fitchel C. E.
Hartman Robert C.
Hunter Stan D.
Kanbach Gottfried
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