Formation of weak Fraunhofer lines of the solar spectrum

Details Formation of weak Fraunhofer lines of the solar spectrum Formation of weak Fraunhofer lines of the solar spectrum

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984azh....61..771b&link_type=abstract

(Astronomicheskii Zhurnal, vol. 61, July-Aug. 1984, p. 771-777) Soviet Astronomy (ISSN 0038-5301), vol. 28, July-Aug. 1984, p. 4

Astronomy and Astrophysics

Astronomy

Fraunhofer Lines, Solar Atmosphere, Solar Spectra, Absorption Spectra, Cerium, Iron, Scattering, Thermodynamic Equilibrium

Scientific paper

The profiles of a number of weak Frauhofer lines of ionized cerium and iron have been calculated with allowance for the combined effects of true absorption and coherent and incoherent scattering. It is shown that separate allowances for the various mechanisms of line formation can lead to significant differences in the profiles. In particular, the central residual line intensities are 4-8 percent greater for true absorption (at the center of the solar disk) than for scattering. Equivalent widths were found to vary by 15-20 percent. Calculations of the contributions of individual scattering mechanisms were also performed for equilibrium and nonequilibrium states. It is found that for weak absorption lines the difference in the central residual line intensities for coherent and incoherent scattering is only 0.2 percent. All the differences were observed to increase toward the edge of the solar disk. On the basis of the theoretical calculations it is concluded that the combined effects of the different mechanisms of line formation and the departure of the level populations from the equilibrium state must be taken into account when calculating Fraunhofer lines.

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