Ultraviolet AL III emission lines and the physics of the solar transition region

Details Ultraviolet AL III emission lines and the physics of the solar transition region Ultraviolet AL III emission lines and the physics of the solar transition region

Apr 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...315l..67d&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 315, April 1, 1987, p. L67-L70. NASA-supported rese

Physics

22

Metallicity, Solar Atmosphere, Solar Spectra, Solar Temperature, Ultraviolet Spectra, Aluminum, Emission Spectra, Solar Physics

Scientific paper

Two lines of the solar UV spectrum were identified as due to 3p-3d Al III transitions near 1612 A; the ratios of these lines to the 3s-3p Al III doublet near 1855 A were found to be very sensitive to temperature. Thus, the temperatures of formation of the Al III lines could be determined by using one of the line ratios in two quiet sun regions, a coronal hole, and an active region. The results were found to be consistent with expectations based on the assumption of ionization equilibrium for Al III. It is suggested that S III lines near 1350 A and 1200 A may also serve as a temperature diagnostic.

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