Chromosphere flare modelsFurther 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.
Document ID
19860065538
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Avrett, E. H. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Kurucz, R. L. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Machado, M. E. (NASA Marshall Space Flight Center Huntsville, AL, United States)