Theoretical line intensities from MG VI, SI VIII, and SX coronal ions

Details Theoretical line intensities from MG VI, SI VIII, and SX coronal ions Theoretical line intensities from MG VI, SI VIII, and SX coronal ions

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.172...47d&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 172, no. 1, Oct. 1990, p. 47-50.

Astronomy and Astrophysics

Astrophysics

Line Spectra, Magnesium, Molecular Ions, Silicon, Solar Corona, Sulfur, Chromosphere, Emission Spectra, Solar Atmosphere, Solar Spectra

Scientific paper

A model of the inner corona, applicable to quite open-field regions and coronal holes is used for computing emission line intensities from Mg VI, Si VIII, and Sx ions of nitrogen sequences. Unlike the original model, the study deals with ions with five levels in the ground term. The computed line intensities indicate that for low-temperature ion Mg VI in the chromosphere-corona transition region, the contrast between the quiet sun and coronal hole regions is not sharp, while for higher-temperature ions Si VIII and Sx, lines formed in the coronal holes are weaker by a factor of two or more compared to lines of the same ion in the quiet-sun regions.

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