Chromosphere flare models

Details Chromosphere flare models Chromosphere flare models

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985smm..conf.....a&link_type=abstract

National Solar Observatory, Solar Maximum Mission Summer Meeting, Sunspot, NM, Aug. 20-24, 1985, Paper. 65 p.

Computer Science

1

Chromosphere, Solar Atmosphere, Solar Flares, Stellar Models, Radiative Transfer, Solar Cooling, Solar Radiation, Solar Spectra, Solar Temperature

Scientific paper

Further calculated results based on the F1 and F2 chromospheric models of Machado et al. (1980) are presented in addition to results from a model with enhanced temperatures relative to the weak-flare model F1 in the upper photosphere and low chromosphere, and from a model with enhanced temperatures relative to the strong flare model F2 in the upper chromosphere. The coupled equations of statistical equilibrium and radiative transfer for H, H(-), He I-II, C I-IV, Si I-II, Mg I-II, Fe, Al, O I-II, Na, and Ca II are solved, and the overall absorption and emission of radiation by lines throughout the spectrum are determined by means of a reduced set of opacities taken from a compilation of over 10 million lines. Semiempirical models show that the white light flare continuum may arise by extreme chromospheric overheating, as well as by an enhancement of the minimum temperature region.

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