Abstract
Results are given of the detailed analysis of fourteen Fe xxv-xxiii lines (λ = 1.850–1.870 Å) in the spectra of a solar flare on 16 Nov. 1970. The spectra were obtained with a resolution of about 4 × 10−4 Å, which revealed lines not previously observed and allowed the measurement of line profiles. The measured values of the wavelengths and emission fluxes are presented and compared with theoretical calculations. The analysis of the contour of the Fe xxv line (λ = 1.850 Å) leads to the conclusion that there is unidirectional macroscopic gas motion in the flare region with the velocity (projection on the line of sight) ≈ ± 90 km s−1.
Measurements of the 8.42 Å Mg xii and 9.16 Å Mg xi lines in the absence of solar flares indicate prolonged existence of active regions on the solar disk with T e = 4−6 × 106K and emission measure ME ≈ 1048 cm−3. The profile of the Mg xii line indicates a macroscopic ion motion with a velocity up to 100 km s−1.
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Grineva, Y.I., Karev, V.I., Korneev, V.V. et al. Solar X-ray spectra observed from the ‘Intercosmos-4’ satellite and the ‘Vertical-2’ rocket. Sol Phys 29, 441–446 (1973). https://doi.org/10.1007/BF00150824
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DOI: https://doi.org/10.1007/BF00150824