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Analysis of the intensities and profiles of the spectral line Mg xii 8.42 Å in the solar X-ray spectrum

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Abstract

High resolution profiles of the Mg xii 8.42 Å line in the solar X-ray spectrum were recorded from the Intercosmos 7 satellite. The Mg xii line intensity provides a sensitive indicator of the hot plasma content (T ≳ 3 × 106 K) in coronal condensations and X-ray flare volumes. The ratio of the line intensity to the intensity of the adjacent continuum has been used to compute approximate thermal models of the emitting regions. For all the investigated coronal condensations the temperature distribution of plasma has been found to be a function monotonically decreasing with temperature. But for some X-ray bursts there occurred a distinct excess of the hot plasma of temperature between 6–10 × 106K. FWHM values of the Mg xii line profiles have been used to estimate ion temperature in the emitting regions.

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Authors and Affiliations

  1. Wroclaw University, Wroclaw, Poland

    J. Jakimiec

  2. Lebedev Physical Institute, Moscow, U.S.S.R.

    V. V. Korneev, V. V. Krutov & I. A. Zhitnik

  3. Polish Academy of Sciences, Solar-Terrestrial Relations Laboratory, Wroclaw, Poland

    S. Pŀocieniak, B. Sylwester & J. Sylwester

Authors
  1. J. Jakimiec
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  2. V. V. Korneev
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  3. V. V. Krutov
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  4. I. A. Zhitnik
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  5. S. Pŀocieniak
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  6. B. Sylwester
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  7. J. Sylwester
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Jakimiec, J., Korneev, V.V., Krutov, V.V. et al. Analysis of the intensities and profiles of the spectral line Mg xii 8.42 Å in the solar X-ray spectrum. Sol Phys 44, 391–401 (1975). https://doi.org/10.1007/BF00153218

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  • DOI: https://doi.org/10.1007/BF00153218

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