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Rocket spectrogram of a solar flare in the 10-100 A region
Acton, L. W.; Bruner, M. E.; Brown, W. A.; Fawcett, B. C.; Schweizer, W.; Speer, R. J.
AA(Lockheed Research Laboratories, Palo Alto, CA), AB(Lockheed Research Laboratories, Palo Alto, CA), AC(Lockheed Research Laboratories, Palo Alto, CA), AD(Science and Engineering Research Council, Rutherford Appleton Laboratory, Didcot, Oxon, England), AE(Fraunhofer Institut für physikalische Messtechnik, Freiburg-im-Breisgau, Germany), AF(Imperial College of Science and Technology, London, England)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 291, April 15, 1985, p. 865-878. Research supported by the Lockheed Independent Research Program and Bundesministerium für Bildung und Wissenschaft. (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Abundance, Solar Flares, Solar Spectra, Solar X-Rays, Spectrograms, Calibrating, Emission Spectra, Line Spectra, Rocket-Borne Instruments, Solar Temperature, Spectrum Analysis, X Ray Spectra, X Ray Telescopes
Bibliographic Code:


The soft (10-100 A) X-ray spectrum of an M-class solar flare was observed with a high-resolution (0.02 A) rocket-borne spectrograph on 1982 July 13. The spectrum samples an area of 600/sq arcsec on the sun, centered on or near the brightest X-ray feature of the flare. Several hundred emission lines characteristic of temperatures from about 0.5 to 7 x 10 to the 6th K have been photographically recorded. All but three of the stronger lines have been identified. It is argued that previous identification of the line at 17.62 A as iron Ly-alpha is incorrect. Spectral lines from nickel, iron, chromium, calcium, sulphur, silicon, aluminium, magnesium, neon, oxygen, nitrogen, and carbon are tabulated and discussed with extensive reference to earlier work. Absolute line intensities are given and the calibration of the telescope-spectrograph is discussed.

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