Observational constraints for a theoretical model describing the soft X-ray flare

Details Observational constraints for a theoretical model describing the soft X-ray flare Observational constraints for a theoretical model describing the soft X-ray flare

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...255..320f&link_type=abstract

Astrophysical Journal, Part 1, vol. 255, Apr. 1, 1982, p. 320-324. NASA-supported research.

Other

26

Chromosphere, Coronal Loops, Solar Flares, Solar X-Rays, Stellar Models, X Ray Spectra, Electron Density (Concentration), Electron Energy, High Resolution, Line Spectra, Solar Atmosphere, Spaceborne Experiments, Spectrum Analysis

Scientific paper

High-resolution solar flare X-ray spectra have recently been obtained from X-ray spectrometer experiments flown on an Air Force spacecraft (P78-1) launched on 1979 February 24. Interpretation of the spectra has produced new results concerning the physical conditions and time behavior of the thermal soft X-ray emitting plasma at temperatures near 20,000,000 K. It is argued that soft and hard X-ray events are not causally related to each other, but are simply two different manifestations of flare energy release. They probably occur in different plasma volumes. The source of the preflare plasma appears to be in the cooler parts of the solar atmosphere, perhaps transition region loops with initial temperatures of 100,000 K and densities of 10 to the 11th per cu cm. Continuous energy input, rather than sequential activation of loops, is required to explain the observations. Compression coupled with chromospheric ablation may produce the high densities in coronal flare loops.

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