A possible explanation of spatial structure of X-rays of at least 100 keV in solar flares observed by the PVO/ISEE 3 spacecraft

Details A possible explanation of spatial structure of X-rays of at least 100 keV in solar flares observed by the PVO/ISEE 3 spacecraft A possible explanation of spatial structure of X-rays of at least 100 keV in solar flares observed by the PVO/ISEE 3 spacecraft

May 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...292..725k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 292, May 15, 1985, p. 725-732. Research supported by the University Grants

Astronomy and Astrophysics

Astrophysics

10

Electron Distribution, Solar Flares, Solar X-Rays, Angular Distribution, Electron Energy, International Sun Earth Explorer 3, Monte Carlo Method, Solar Atmosphere

Scientific paper

Evolution of electron energy and angular distributions in the solar atmosphere has been studied for large deflections by combining small-angle analytical treatment with Monte Carlo technique. The incident electron energies are 60, 100, and 300 keV having incidence angles of 0, 30, and 60 degrees in the beginning. The change in electron spectral index with height has been studied. Using these distributions the bremsstrahlung X-ray flux ratio due to 60-degree and 0-degree electron incidence angles was computed for different photon energies with height and the results are compared with observations of Kane et al. The calculated flux ratio corresponds well with the observations and reproduces well the rise time of X-ray flux of Kane and Anderson.

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