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Arking, A., and J. Herring, 1963: The contribution of absorption lines to the opacity of matter in stellar interiors. Publ. Astron. Soc. Pacific, 75, 226-235.
The structure and evolution of stars depends very sensitively on the opacity of the matter throughout the star. For stars of the sun's mass and greater, the bulk of the material is at temperatures above a million degrees, and an accurate knowledge of opacities at these temperatures is important for calculating the time scales of various phases of stellar evolution.
This paper reports a calculation of the contribution of the lines to the opacity of stellar material at conditions typical of stellar interiors (temperatures of 1 to 20×106 °K and electron densities of ~3×1025/m3). Our results indicate that the total Rosseland mean opacity is increased by ~ 10 to 40 percent above the continuous opacity for the Keller and Meyerott Group X mixture of e1ements.l The mass fractions of this mixture are hydrogen (.485), helium (.485), and heavier elements (.03) ; of the heavier elements the most important, at the temperatures under consideration, are iron, potassium, and aluniinum.
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