Asymmetry of Absorption Lines in the Solar and Procyon Sprecta
The comparative analysis of solar and Procyon spectral line bisectors is carried out. The interpretation of the basic features of solar and Procyon spectral line bisectors is given on the basis of the theoretical inhomogeneous models of their atmospheres and also on the basis of stochastic approximation theory of spectral line formation. The conclusion is made that the main differences between the Sun and Procyon are caused by the differences of correlation between of the temperature and vertical velocity fluctuations in their atmospheres.
KeywordsSpectral Line Magnetic Tape Line Bisector Solar Photosphere Iron Line
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- Delbouille L.,Neven L.,Roland C, 1973, Photometric Atlas of Solar Spectrum from 3000 to 10000 A, LiegeGoogle Scholar
- Gadun A.S. 1986, Preprint ITP of Ac.Sc.Ukr,SSR,ITF-86-106RGoogle Scholar
- Griffin R,,Griffin R, 1979, A Photometric Atlas of the Spectrum of Procyon 3140 - 7470 A, CambridgeGoogle Scholar
- Kurucz R.L.,Furenlid J.,Brault J,,Testernan L, 1984, Solar Flux Atlas from 290 to 1300 nm, Harvard UniversityGoogle Scholar