Fe XXIII 263 A and Fe XXIV 255 A emission in solar flares

Details Fe XXIII 263 A and Fe XXIV 255 A emission in solar flares Fe XXIII 263 A and Fe XXIV 255 A emission in solar flares

Apr 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...197l..33w&link_type=abstract

Astrophysical Journal, vol. 197, Apr. 1, 1975, pt. 2, p. L33-L35.

Astronomy and Astrophysics

Astronomy

48

Ferric Ions, Line Spectra, Solar Flares, Spaceborne Astronomy, Ultraviolet Spectra, Luminous Intensity, Skylab Program, Solar Spectra, Spectroheliographs

Scientific paper

The 263.7-A line observed in solar flare spectra during the Skylab mission is identified as an intercombination line of Fe XXIII. The identification is confirmed by direct observation of the line along the isoelectronic sequence, including S XIII, Ar XV, Ca XVII, and Cr XXI. Observation of the beryllium sequence in solar flares is outlined, and the method of identification is described. Significant characteristics of the Fe XXIII and Fe XXIV images observed in the flare of June 15, 1973, are discussed and include an archlike spatial structure spanning the magnetic neutral line and a Doppler-widened emission core, which may pinpoint the site of the energy release.

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