Titlebook: CNO Isotopes in Astrophysics; Proceedings of a Spe Jean Audouze Conference proceedings 1977 D. Reidel Publishing Company, Dordrecht,Holland

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Carbon and Nitrogen Abundances in Giant Stars of the Metal Poor Globular Cluster M92 — A Preliminaryassociates and students. In summarizing these results, Dearborn, Eggleton, and Schramm (1976) concluded that in the atmospheres of pre-He-core flash red giants there is evidence for substantial depletion of C. and enhancement of C. presumably as a result of deep mixing of envelope material into laye

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CNO Isotopes and Red Giants stage, molecular lines are observed from which CNO isotope ratios and abundances can be determined. It is also during this stage that a surface convection zone penetrates into the interior mixing out material which was processed via the CNO tricycle (Iben 1964, 1966). Comparison of observed isotope

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Abundance of Carbon in NGC 7027 in grains and the amount in a gaseous form. Here we present the most relevant results and discuss some implications on the late stages of the stellar evolution and the chemical evolution of the Galaxy.

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The CNO Composition in Novae Envelopeonuclear runaway and ejection of a sizeable fraction of the envelope. Recently extensive numerical calculations of this model were carried out by Starrfield, Sparks and Truran (1974) (SST). In these calculations the assumed initial model is a degenerate carbon core of 1M☉. with an envelope of (1.25

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17O and 18O Abundances in Interstellar CloudsO is so widespread in our Galaxy, its isotopic substitutions are of particular importance. We concentrate here on the two isotopic molecules .C.O and .C.O. They give only faint J = 1 - 0 lines, at 112.36 GHz and 109.78 GHz respectively, but these lines are unsaturated even in Sgr B2 (as can be check