The curve of growth for the sun as a star in the Milne-Eddington approximation

Details The curve of growth for the sun as a star in the Milne-Eddington approximation The curve of growth for the sun as a star in the Milne-Eddington approximation

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988azh....65..613k&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 65, May-June 1988, p. 613-620. In Russian.

Astronomy and Astrophysics

Astronomy

Eddington Approximation, Milne Method, Solar Spectra, Stellar Evolution, Sun, Abundance, Iron, Photosphere, Spectral Line Width, Stellar Atmospheres

Scientific paper

For the first time, the experimental curve of growth for the Sun as a star has been constructed in the Milne-Eddington approximation, basing on the Fe I lines. The cleanest 280 Fe I lines in the spectral region from λ4000 Å to λ7000 Å have been used. The equivalent widths have been taken from the works of Rutten and van der Zalm who had published a list of 602 clean (unblended) lines in the spectrum of the Sun as a star from Becker et al.'s atlas. Kostyk's system of absolute oscillator strengths was used. The velocity of microturbulent motion (vm = 1±0.3 km/s), excitation temperature (Tex = 5360±70K) and iron abundance (lg NFe = 7.57±0.10) in the photosphere of the Sun as a star were determined.

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