Analysis of the intensities and profiles of the spectral line Mgxii8.42 Å in the solar X-ray spectrum

✍ Scribed by J. Jakimiec; V. V. Korneev; V. V. Krutov; I. A. Zhitnik; S. Pŀocieniak; B. Sylwester; J. Sylwester

• Publisher: Springer
• Year: 1975
• Tongue: English
• Weight: 424 KB
• Volume: 44
• Category: Article
• ISSN: 0038-0938
• DOI: 10.1007/bf00153218

✦ Synopsis

High resolution profiles of the Mg xn 8.42 A line in the solar X-ray spectrum were recorded from the Intercosmos 7 satellite. The Mg xaI line intensity provides a sensitive indicator of the hot plasma content (T > 3 • 106K) 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 xtt line profiles have been used to estimate ion temperature in the emitting regions.