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Title:
Solar flare X-ray spectra from the Solar Maximum Mission Flat Crystal Spectrometer
Authors:
Phillips, K. J. H.; Fawcett, B. C.; Kent, B. J.; Gabriel, A. H.; Leibacher, J. W.; Wolfson, C. J.; Acton, L. W.; Parkinson, J. H.; Culhane, J. L.; Mason, H. E.
Affiliation:
AA(Science Research Council, Rutherford and Appleton Laboratories, Didcot, Oxon, England), AB(Science Research Council, Rutherford and Appleton Laboratories, Didcot, Oxon, England), AC(Science Research Council, Rutherford and Appleton Laboratories, Didcot, Oxon, England), AD(Science Research Council, Rutherford and Appleton Laboratories, Didcot, Oxon, England), AE(Lockheed Research Laboratories, Palo Alto, CA), AF(Lockheed Research Laboratories, Palo Alto, CA), AG(Lockheed Research Laboratories, Palo Alto, CA), AH(London, University College, Dorking, Surrey, England), AI(London, University College, Dorking, Surrey, England), AJ(Cambridge University, Cambridge, England)
Publication:
Astrophysical Journal, Part 1, vol. 256, May 15, 1982, p. 774-787. Research supported by the Science Research Council and Lockheed Independent Research Program; (ApJ Homepage)
Publication Date:
05/1982
Category:
Solar Physics
Origin:
STI
NASA/STI Keywords:
ELECTRON DENSITY (CONCENTRATION), SOLAR FLARES, SOLAR MAXIMUM MISSION, SOLAR SPECTRA, SOLAR X-RAYS, X RAY SPECTRA, HIGH RESOLUTION, LINE SPECTRA, SPECTRUM ANALYSIS, VOIGT EFFECT
Comment:
A&AA ID. AAA031.073.037
DOI:
10.1086/159950
Bibliographic Code:
1982ApJ...256..774P

Abstract

High-resolution solar X-ray spectra obtained with the Flat Crystal Spectrometer aboard the Solar Maximum Mission from two solar flares and a nonflaring active region are analyzed. The 1-22 A region was observed during the flare on 1980 August 25, while smaller spectral regions were repeatedly covered during the 1980 November 5 flare. Voigt profiles were fitted to spectral lines to derive accurate wavelengths and to resolve blends. During the August 25 flare, 205 lines were found in the range 5.68-18.97 A, identifications being provided for all but 40 (mostly weak) lines. Upper limits to flare densities are derived from various line ratios, the hotter (about 10 to the 7th K) ions giving an electron density of less than 10 to the 12th per cu cm for the August 25 flare. Other observed line ratios (e.g., in Fe XVII and Mg XII) indicate a need for revisions in theoretical calculations.

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