Abstract
Statistical data for line blanketing in the solar atmosphere have been extracted from the Revised Rowland Table. The data are corrected for apparent observational incompleteness due to line crowding and blending and are placed in a convenient form for calculations. An attempt is made to interpret the data in terms of schematic representations of the energy levels and distribution of gf-values for the important absorbers. The analysis leads to predictions in good agreement with the forms of the statistical data and substantiates the assumption of observational incompleteness in the original data. The analysis suggests that the solar data may provide useful guidance in the blanketing of stellar atmospheres sufficiently close to solar type.
A blanketing method is presented which makes use of a uniformly-smeared-line (single picket) procedure and which assumes LTE and a weak-line curve of growth. The blanketing coefficient is obtained in a simple manner from the corrected statistical data and is both depth and wavelength dependent. An alternative method utilizing a four-picket scheme and average absorption coefficient profiles is suggested. Comparison of solar models computed by the two methods shows good agreement and gives support for the smeared-line procedure. Comparison of the solar model with a non-LTE blanketed model of Athay also shows reasonable agreement.
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Publications of the Goethe Link Observatory, Indiana University, No. 110.
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Mutschlecner, J.P., Keller, C.F. Semi-empirical solar line blanketing. Sol Phys 14, 294–309 (1970). https://doi.org/10.1007/BF00221315
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DOI: https://doi.org/10.1007/BF00221315