Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.106..283m&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 106, no. 2, Nov. 1984, p. 283-297. Research supported by the Ohio State Un
Astronomy and Astrophysics
Astrophysics
18
Polarized Radiation, Radiative Transfer, Solar Spectra, Stellar Atmospheres, Stellar Radiation, Calcium, Potassium, Resonance Lines, Spectral Line Width, Strontium
Scientific paper
McKenna's (1981, 1984) method is used to compute the polarization structure in several spectral lines of solar type stars, employing a frequency distribution function that is a linear combination of R(II) and R(III). The line profiles and polarization structures, as well as the center-to-limb behavior of the line center polarization, are noted to be in good agreement with observations. It is also found that, for strong resonance lines, the proper redistribution function is a linear combination of R(III) and R(V). The primary reason for this is that both the upper and lower levels are broadened by collisions in this case, thereby violating the assumptions on which the redistribution functions R(II) and R(III) are based.
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