Elemental abundances in different solar regions from EUV observations

Details Elemental abundances in different solar regions from EUV observations Elemental abundances in different solar regions from EUV observations

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...198..311n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 198, no. 1-2, June 1988, p. 311-321. Research supported by the Ministero della

Astronomy and Astrophysics

Astrophysics

9

Abundance, Extreme Ultraviolet Radiation, Solar Corona, Carbon, Coronal Holes, Magnesium, Neon, Nitrogen, Oxygen, Silicon, Sulfur

Scientific paper

The relative abundances of C, N, O, Ne, Mg, Si, S in different regions of the solar transition zone (a coronal hole, a quiet and an active region) have been determined from the analysis of average EUV spectra in the range 296-1350 A. The methodology described by Pottasch (1964) and later on improved (Dupree, 1972; Withbroe, 1981) has been used; moreover, the role played by the population of the metastable levels of the emitting ions has been taken into account. The abundances found in different regions and those found at the photospheric level do not differ more than the errors, except for oxygen, whose abundances seem to be lower for values of T less than 10 exp 5.2 K, particularly in the active region. The comparison between quiet region and coronal hole shows that their chemical compositions differ by values much lower than the estimated uncertainty, which suggests that the errors affecting the abundance determinations are lower than estimated. This could imply that differences in the chemical composition between active region and other coronal regions exist.

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