On the Fe XXIV emission in the solar flare of 1973 June 15

Details On the Fe XXIV emission in the solar flare of 1973 June 15 On the Fe XXIV emission in the solar flare of 1973 June 15

Dec 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974apj...194l.111w&link_type=abstract

Astrophysical Journal, vol. 194, Dec. 1, 1974, pt. 2, p. L111-L113.

Astronomy and Astrophysics

Astronomy

62

Emission Spectra, Far Ultraviolet Radiation, Iron, Line Spectra, Solar Flares, Spectroheliographs, Apollo Telescope Mount, Astronomical Spectroscopy, Skylab Program, Solar Corona, Solar Spectra, Spaceborne Astronomy

Scientific paper

The double ribbon flare of 1973 June 15 was observed in the XUV wavelength region with the NRL objective grating spectroheliograph during the Skylab missions. The Fe XXIV emissions at 192.1 and 255.2 A are prominent in the early phase of the flare. The Fe XXIV emission is centered over the neutral line, forming a bridgelike structure between magnetic regions of opposite polarity. This is unlike the emission pattern of He II, the transition zone ions, and Fe IX-XVI, which are relatively brighter in the adjacent flare ribbons overlying strong vertical magnetic field. An electron density of 5 times 10 to the 10th per cu cm for the Fe XXIV emission region is deduced from the observational data, and the cooling rate is briefly discussed.

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