The Broadening of Metallic Lines in Cool Stars
A theory for the broadening of spectral lines by collisions with atomic hydrogen developed by Anstee and O’Mara  is described and when applied to strong lines of elements in the sun leads to abundances which are independent of non-thermal motions in the photosphere and in excellent agreement with meteoritic values. In the case of the solar abundance of iron the results lead to a resolution of recent conflict concerning possible differences between the abundance of iron in the sun and meteorites. Excellent results obtained with the Mg b-lines permit these lines to be used in abundance determinations in other stars and also makes them particularly useful in determining the temperature structure in cool stars.
KeywordsInteraction Energy Strong Line Radial Wave Function Cool Star Solar Abundance
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- 4.Ross J. E. Spectrum synthesis program.http://www.uq.edu.au/~phjross/syn.htm.