Morphology of the 10 Million Degree Plasma in Solar Flares and the Failure of the Chromospheric Evaporation Model

Details Morphology of the 10 Million Degree Plasma in Solar Flares and the Failure of the Chromospheric Evaporation Model Morphology of the 10 Million Degree Plasma in Solar Flares and the Failure of the Chromospheric Evaporation Model

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994kofu.symp..177s&link_type=abstract

In: Proceedings of Kofu Symposium, Kofu, Japan, Sept. 6-10, 1993, p.177-180.

Computer Science

3

Scientific paper

The SXT images of over fifty C, M, and X type flares which occurred between October 1991 and February 1993 were analyzed. For each flare, the 10 million degree emitting region was typically found to be located at the loop top in the first well-exposed flare image recorded during the rise phase (within 1 to 2 minutes after flare onset), in images recorded near the intensity peak, and in images recorded during most of the decay phase. For the November 2 1992 limb flare, the loop top was bright for 24 hours. For a few flares, the brightness of the footpoints in the onset images was comparable to the brightness of the loop top, but the loop top brightness rapidly increased relative to the footpoints and remained intense for the duration of the flare. The brightest region at the loop top was very small throughout the flare, often as small as a single pixel (1800x1800 km). The conclusions are that the energy is deposited in a small volume at the top of the flaring loop structure, the heating mechanism acts over a period of up to tens of hours, and the hot plasma is confined at the top of the loop structure. These results are not explained by the traditional chromospheric evaporation model of solar flares.

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