Statistics – Computation
Scientific paper
Nov 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...381..572m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 381, Nov. 10, 1991, p. 572-577. Research supported by U.S. Navy.
Statistics
Computation
14
Electron Beams, Solar Flares, Solar X-Rays, X Ray Sources, Computational Astrophysics, Digital Simulation, Emission Spectra
Scientific paper
Using time-dependent numerical simulations and Solar Maximum Mission observations of a solar flare on 1985 January 23, a study is conducted of the ability of an electron-beam-heating model to reproduce the rise phase of a flare as observed in soft X-ray lines of Ca XIX. The electron beam is parameterized by a peak flux, a low-energy cutoff, and a spectral index, and has a time dependence similar to the observed hard X-ray burst. For a spectral index of 6, only models with a low-energy cutoff of 20 keV reproduce the observed peak emission in the Ca XIX line complex. All models with a low-energy cutoff of 15 keV produce too much emission, while all models with a 25-keV cutoff too little emission. None of the models reproduces the temporal behavior of the soft X-ray emission. The electron-beam-heated component is theorized to only represent a small fraction of the energy released in the impulsive phase of this flare.
Mariska John T.
Zarro Dominic M.
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