Electron Densities in the Coronae of the Sun and Procyon from Extreme-Ultraviolet Emission Line Ratios in Fe XI

Details Electron Densities in the Coronae of the Sun and Procyon from Extreme-Ultraviolet Emission Line Ratios in Fe XI Electron Densities in the Coronae of the Sun and Procyon from Extreme-Ultraviolet Emission Line Ratios in Fe XI

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...562..566p&link_type=abstract

The Astrophysical Journal, Volume 562, Issue 1, pp. 566-574.

Astronomy and Astrophysics

Astronomy

3

Atomic Data, Line: Identification, Stars: Individual (Procyon, Α Canis Minoris), Sun: Corona, Sun: Uv Radiation

Scientific paper

New R-matrix calculations of electron impact excitation rates for Fe XI are used to determine theoretical emission line ratios applicable to solar and stellar coronal observations. These are subsequently compared to solar spectra of the quiet Sun and an active region made by the Solar EUV Rocket Telescope and Spectrograph (SERTS-95), as well as Skylab observations of two flares. Line blending is identified, and electron densities of 109.3, 109.7, >=1010.8, and >=1011.3 cm-3 are found for the quiet Sun, active region, and the two flares, respectively. Observations of the F5 IV-V star Procyon, made with the Extreme Ultraviolet Explorer (EUVE) satellite, are compared and contrasted with the solar observations. It is confirmed that Procyon's average coronal conditions are very similar to those seen in the quiet Sun, with Ne=109.4 cm-3. In addition, although the quiet Sun is the closest solar analog to Procyon, we conclude that Procyon's coronal temperatures are slightly hotter than solar. A filling factor of 25+38-12% was derived for the corona of Procyon.

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