Comparison of theoretical AR XV line strengths with SKYLAB XUV observations of solar flares

Details Comparison of theoretical AR XV line strengths with SKYLAB XUV observations of solar flares Comparison of theoretical AR XV line strengths with SKYLAB XUV observations of solar flares

Sep 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988iraj...18..267m&link_type=abstract

(Astronomocal Science Group of Ireland, Meeting, University College, Cork, Republic of Ireland, Mar. 31, 1988) Irish Astronomica

Astronomy and Astrophysics

Astrophysics

Argon, Line Spectra, Skylab Program, Solar Flares, Ultraviolet Spectra, Atomic Energy Levels, Atomic Excitations, Electron Transitions, Emission Spectra, Solar Corona

Scientific paper

The UV emission of the six energetically lowest LS states of AR XV has been observed in high-temperature laboratory and astrophysical plasmas. The Skylab-observed line intensity ratio I(212.12)/I(423.98) for the solar flare of August 9, 1973 is found to be within 25 percent of the theoretical value of 47.5 at the temperature of the maximum Ar XV fractional abundance in ionization equilibrium. Observational data for the ratio I(221.12)/I(266.23) are found to be inconsistent with the value of N(e) = 10 to the 11th/cu cm derived from the Ca XVII line strengths in the same flare by Keenan et al. (1988).

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