Abstract
The data from OGO-5 and OSO-7 X-ray experiments have been compared with optical data from six chromospheric flares with filament disruption associated with slow thermal X-ray bursts. Filament activation accompanied by a slight X-ray enhancement precedes the first evidence of Hα flare by a few minutes. Rapid increase of the soft X-ray flux accompanies the phase of fastest expansion of the filament. Plateau or slow decay phases in the X-ray flux are associated with slowing and termination of filament expansion. The soft X-ray flux increases as F∼(A + Bh) h, where h is the height of the disrupted prominence at any given time and A and B are constants. We suggest that the soft X-ray emission originates from a growing shell of roughly constant thickness of high-temperature plasma due to the compression of the coronal gas by the expanding prominence.
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Part of this work was carried out while at Big Bear Solar Observatory, CALTECH, Pasadena, California, U.S.A.
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Roy, JR., Tang, F. Slow X-ray bursts and flares with filament disruption. Sol Phys 42, 425–439 (1975). https://doi.org/10.1007/BF00149923
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DOI: https://doi.org/10.1007/BF00149923