A semiempirical model of the upper flare chromosphere

Details A semiempirical model of the upper flare chromosphere A semiempirical model of the upper flare chromosphere

Mar 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...228..598l&link_type=abstract

Astrophysical Journal, Part 1, vol. 228, Mar. 1, 1979, p. 598-609.

Astronomy and Astrophysics

Astrophysics

49

Atmospheric Models, Chromosphere, Line Shape, Solar Atmosphere, Solar Flares, Ultraviolet Spectra, H Lines, Radiative Transfer, Solar Temperature, Spectroheliographs, Temperature Profiles

Scientific paper

Ultraviolet spectra of the August 9, 1973, flare taken with the NRL S082B spectrograph aboard ATM/Skylab have been analyzed to derive a semiempirical model of the flare chromosphere between 5500 and 100,000 K. The hydrogen radiative transfer is solved to obtain a self-consistent set of physical conditions within the flare atmosphere, from which line profiles and continua of the ions C I, C II, C III, and C IV are synthesized and compared with the observations. The model exhibits a rapid rise in the temperature at a column mass of 0.0003 g/sq cm. There is some evidence for much of the C III line emission's arising from flare kernels not exceeding 3 arcsec in size, and the C IV line profiles indicate the possibility of nonequilibrium excitation.

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