Impulsive phase of flares in soft X-ray emission

• Published in: Solar physics 1982-05, Vol.78 (1), p.107-123
• Main Authors: Antonucci, E., Gabriel, A. H., Acton, L. W., Culhane, J. L., Doyle, J. G., Leibacher, J. W., Machado, M. E., Orwig, L. E., Rapley, C. G.
• Format: Article
• Language: English
• ISSN: 0038-0938; 1573-093X
• DOI: 10.1007/BF00151147

Observations made by using the bent crystal spectrometer instrument on the Solar Maximum Mission show that turbulence and blue-shifted motions are characteristic of the soft X-ray plasma during the impulsive phase of flares and are coincident with the hard X-ray bursts observed by the hard X-ray burst spectrometer. A method for analyzing the Ca XIX and Fe XXV spectra characteristic of the impulsive phase is presented. Nonthermal widths and blue-shifted components in the spectral lines of Ca XIX and Fe XXV indicate the presence of turbulent velocities exceeding 100 km sec super(-) super(1) and upward motions of 300-400 km sec super(-) super(1) . The April 10, May 9, and June 29, 1980, flares are studied. Detailed study of the geometry of the region, inferred from the flat crystal spectrometer measurements and the image of the flare detected by the hard X-ray imaging spectrometer, shows that the April 10 flare has two separated footpoints bright in hard X-rays. Plasma heated to temperatures greater than 10 super(7) K rises from the footpoints. During the 3 min. in which the evaporation process occurs, an energy of 3.7 x 10 super(3) super(0) ergs is deposited in the loop. At the end of the evaporation process, the total energy observed in the loop reaches its maximum value of 3 x 10 super(3) super(0) ergs. This is consistent with the above figures, permitting loss by radiation and conduction. Thus, the energy input caused by the blue-shifted plasma flowing into the flaring loop through the footpoints can explain the thermal and turbulent energy accumulated in this region during the impulsive phase.