On the determination of carbon isotopic ratios in cool carbon stars
II. Accuracy of the iso-intensity method for crowded spectra
Received 5 March 1999 / Accepted 26 March 1999
de Laverny & Gustafsson (1998, Paper I) questioned the iso-intensity method used by Ohnaka & Tsuji (1996) to derive carbon isotopic ratios in cool carbon stars. As a reply, Ohnaka & Tsuji (1998) pointed out that the method criticized in Paper I differs from the original one and conclude that our results are unreliable. No comparison of the two methods was, however, made. The iso-intensity method used in Paper I and OT96 do slighty differ in their definition. In investigating the consequences of this difference we have found that they are rather insignificant. We therefore confirm that the iso-intensity method is not reliable when applied to crowded spectra of cool stars. That reinforces the conclusions presented in Paper I.
Key words: stars: abundances stars: late-type stars: AGB and post-AGB stars: carbon molecular processes
Send offprint requests to: P. de Laverny (email@example.com)
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© European Southern Observatory (ESO) 1999
Online publication: May 21, 1999