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  • 1
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    Great microwave bursts and hard X-rays from solar flares (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: In the present study of the microwave and hard X-ray characteristics of 13 solar flares emitting microwave fluxes greater than 500 solar flux units, simultaneous 3-35 GHz and hard X-ray observations were conducted in the 30-500 keV energy range. An analysis is conducted to determine whether the same distribution of energetic electrons can explain both emissions; tests for any correlations between them yield results suggesting that optically thick microwave emission, near the peak frequency, originates in the same electron population that produces the hard X-rays. A single temperature model and a multitemperature model were tested for consistency with the coincident X-ray and microwave spectra at microwave burst maximum; neither model, however, attempts to explain the high frequency component of the microwave spectrum.
    Keywords: SOLAR PHYSICS
    Type: Solar Physics (ISSN 0038-0938); 96; 339-356
    Format: text
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    NASA TECHNICAL REPORTS
  • 2
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    Great microwave bursts and hard X-rays from solar flares (1983)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The microwave and hard X-ray charateristics of 13 solar flares that produced microwave fluxes greater than 500 Solar Flux Units were analyzed. These Great Microwave Bursts were observed in the frequency range from 3 to 35 GHz at Berne, and simultaneous hard X-ray observations were made in the energy range from 30 to 500 keV with the Hard X-Ray Burst Spectrometer on the Solar Maximum Mission spacecraft. The principal aim of this analysis is to determine whether or not the same distribution of energetic electrons can explain both emissions. Correlations were found between respective temporal characteristics and, for the first time, between microwave and hard X-ray spectral characteristics. A single-temperature and a multi-temperature model from the literature were tested for consistency with the coincident X-ray and microwave spectra at microwave burst maximum. Four events are inconsistent with both of the models tested, and neither of the models attempts to explain the high-frequency part of the microwave spectrum. A model in which the emissions above and below the peak frequency originate in two different parts of a diverging magnetic loop is proposed. With this model the entire microwave spectrum of all but one of the events is explained.
    Keywords: SOLAR PHYSICS
    Type: NASA-TM-85052 , NAS 1.15:85052
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 3
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    Composition and spectrum of particles with 0.2 or = E or = 30 MeV/nuc in the 25 January 1971 solar flare (1971)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Keywords: SOLAR PHYSICS
    Type: Res. in the Space Sci., v. 2; 6 p
    Format: text
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    NASA TECHNICAL REPORTS
  • 4
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    Solar flare particles - Energy-dependent composition and relationship to solar composition (1975)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Plastic and glass track detectors on rockets and Apollo spacecraft have been used to determine the composition of particles from He to Ni at energies from 0.1 to 50 MeV per nucleon in several solar flares of widely varying intensities. At low energies the composition of solar particles is enriched in heavy elements by an amount, relative to the asymptotic high-energy composition, that increases with atomic number from Z = 2 up to at least Z = 50, that decreases with energy, and that varies from flare to flare. At high energies (usually beyond an energy of 5 to 20 MeV per nucleon) the composition becomes independent of energy and, though somewhat variable from flare to flare, approximates the composition of the solar atmosphere. A table of abundances of the even-Z elements from He to Ni (plus N) in solar particles is constructed by averaging the asymptotic high-energy abundances in several flares.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal; 195; Jan. 1
    Format: text
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    NASA TECHNICAL REPORTS
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