Analysis of a Series of Solar Flare X-Ray Spectra.
AEROSPACE CORP EL SEGUNDO CA SPACE SCIENCES LAB
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We analyze thirteen X-ray line spectra 7.8-23.0 A acquired during a solar flare that peaked at 2326 UT on 1979 March 31. The data include fluxes of lines excited throughout the temperature range 2-18 million K, the entire range present in the coronal flare. The coronal flare emission measure began to decrease 500 s or less after the broad band X-ray flux peaked. We construct the differential emission measure epsilonT for 2-18 million K from the data by using collision strengths now available for a small number of the observed lines. The total emission measure for T greater than 2 million K, the radiative energy loss rate, the density at 2 million K, and the conductive cooling time are derived from the data, but lack of information on electron densities prevents a detailed study of the flare energetics. This situation is unlikely to improve in the near future. Conductive cooling was more important than radiative cooling for coronal temperatures in this flare. Author