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Solar neutron emissivity during the large flare on 1982 June 3
Chupp, E. L.; Debrunner, H.; Flueckiger, E.; Forrest, D. J.; Golliez, F.; Kanbach, G.; Vestrand, W. T.; Cooper, J.; Share, G.
AA(New Hampshire, University, Durham), AB(New Hampshire, University, Durham), AC(Bern, Universität, Switzerland), AD(Bern, Universität, Switzerland), AE(Bern, Universität, Switzerland)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 318, July 15, 1987, p. 913-925. USAF-supported research. (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Emission Spectra, Neutron Emission, Neutron Spectra, Particle Acceleration, Solar Corpuscular Radiation, Solar Flares, Solar Neutrons, Bessel Functions, Gamma Ray Spectrometers, Neutron Decay, Neutron Flux Density, Solar Atmosphere, Solar Maximum Mission, Time Measurement
Bibliographic Code:


For the solar neutron event on June 3, 1982, it is shown here that the combined SMM Gamma Ray Spectrometer and Jungfraujoch neutron monitor data require a time-extended emission of neutrons at the sun with energies of 100 MeV to about 2 GeV. The solar neutron emissivity spectrum is shown to have a strong downward curvature or truncation between 2 and 4 GeV. A Bessel function and truncated power law give acceptable fits to the observational data, but only the power law can explain the rapid rise of the neutron monitor count rate. The integrated emissivity of neutrons above E(n) of 100 MeV is strongly constrained at 8 x 10 to the 28th neutrons/sr and is essentially independent of neutron spectral shape. At neutron energies of about 100 MeV, good agreement is found for both spectral forms with observations of neutron decay protons.

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