Numerical simulations of loops heated to solar flare temperatures. III - Asymmetrical heating

Details Numerical simulations of loops heated to solar flare temperatures. III - Asymmetrical heating Numerical simulations of loops heated to solar flare temperatures. III - Asymmetrical heating

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...286..787c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 286, Nov. 15, 1984, p. 787-803. NASA-Navy-supported research.

Astronomy and Astrophysics

Astrophysics

48

Coronal Loops, Hydrodynamics, Plasma Heating, Solar Flares, Chromosphere, Evaporation, Gas Flow, Iron, Line Spectra, Solar Spectra, Solar X-Rays, Ultraviolet Spectra, Velocity Distribution

Scientific paper

A numerical model is defined for asymmetric full solar flare loop heating and comparisons are made with observational data. The Dynamic Flux Tube Model is used to describe the heating process in terms of one-dimensional, two fluid conservation equations of mass, energy and momentum. An adaptive grid allows for the downward movement of the transition region caused by an advancing conduction front. A loop 20,000 km long is considered, along with a flare heating system and the hydrodynamic evolution of the loop. The model was applied to generating line profiles and spatial X-ray and UV line distributions, which were compared with SMM, P78-1 and Hintori data for Fe, Ca and Mg spectra. Little agreement was obtained, and it is suggested that flares be treated as multi-loop phenomena. Finally, it is concluded that chromospheric evaporation is not an effective mechanism for generating the soft X-ray bursts associated with flares.

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