A common model for solar filigree and faculae

Details A common model for solar filigree and faculae A common model for solar filigree and faculae

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....75..263s&link_type=abstract

Astronomy and Astrophysics, vol. 75, no. 3, June 1979, p. 263-267.

Astronomy and Astrophysics

Astrophysics

18

Atmospheric Models, Faculae, Line Shape, Photosphere, Solar Atmosphere, Zeeman Effect, Abundance, Electrophotometry, Iron, Line Spectra, Solar Limb, Solar Spectra, Stellar Models, Titanium

Scientific paper

A disk-center filigree model for facular plages is examined by using photographic spectra of solar lines with a reasonably small Zeeman splitting. The results fully confirm previously reported line weakenings as well as a previously observed decrease in the line weakenings toward the limb. It is found that the highly excited lines of Fe II at 5264 A, Ti II at 4568 A, and Si I at 6145 A exhibit line strengthenings for most limb faculae but that the absolute intensities of the line cores are always higher than those of the neighboring photosphere. Photoelectric measurements of the wavelength dependence of the contrast in true continuum windows and in facular spectra obtained at various heliocentric angles reveal that the contrast decreases with wavelength, as reported earlier.

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