Coronal abundances in solar active regions measured by the Solar Maximum Mission flat crystal spectrometer

Details Coronal abundances in solar active regions measured by the Solar Maximum Mission flat crystal spectrometer Coronal abundances in solar active regions measured by the Solar Maximum Mission flat crystal spectrometer

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.348..347s&link_type=abstract

In ESA, Proceedings of the First SOHO Workshop: Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition p 347-3

Computer Science

13

Plasma Composition, Solar Activity, Solar Corona, Solar Maximum Mission, Solar Spectrometers, Abundance, Iron, Line Spectra, Magnesium, Neon, Oxygen

Scientific paper

High resolution soft X-ray spectra acquired by the Flat Crystal Spectrometer (FCS) on solar Maximum Mission provide an excellent data base to study the relative abundances of O, Ne, Mg, and Fe in solar active regions. The FCS data show significant variability for all combinations of these elements. The largest variation occurs for Fe:Ne, which shows region to region changes of up to a factor of 7, and frequent factor of 2 variations in day to day samples of a given region. The atomic data and the ionization balance calculations used to interpret the line ratios affect the actual abundance values obtained, but have little effect on the magnitude of the total range of variation inferred. Resonance scattering of Fe XVII could cause a systematic offset in the abundances determined, but cannot be responsbile for the bulk of the observed variability. While abundance variability complicates the derivation of plasma parameters from spectroscopic measurements, it should offer exciting new clues to the processes which form and heat the corona.

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