Abstract
A large-area high-sensitivity X-ray spectrometer has been constructed and used to measure the 1.8–5.3 Å X-ray emission of the Sun under quiescent conditions. The instrument utilizes Bragg reflection from mosaic graphite crystals. The data indicate that the X-ray emission can best be accounted for by a multitemperature model of the solar atmosphere in which both the over-all corona and active regions contribute to the X-ray spectrum. Theoretical calculations of the X-ray flux of a hot, optically thin plasma have been used to estimate the solar conditions at the time when the measurements were made.
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References
Culhane, J. L. and Acton, L. W.: 1970, Monthly Notices Roy. Astron. Soc. 151, 141.
Kestenbaum, H.: 1972, Ph.D. Thesis, Columbia University, New York, N. Y.
Kestenbaum, H.: 1973, Appl. Spectry. 27, 454.
Landini, M. and Fossi, B. C. Monsignori: 1970, Astron. Astrophys. 6, 468.
Mewe, R.: 1972, Solar Phys. 22, 459.
Neupert, W.: 1972, private communication.
Tucker, W. H. and Koren, M.: 1971, Astrophys. J. 168, 283.
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Wolff, R.S. Measurement of the X-ray emission of the solar atmosphere during a period of low activity. Sol Phys 34, 163–172 (1974). https://doi.org/10.1007/BF00149607
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DOI: https://doi.org/10.1007/BF00149607