CNO Isotopes in Astrophysics: Proceedings of a Special IAU by Jean Audouze (auth.), Jean Audouze (eds.)

By Jean Audouze (auth.), Jean Audouze (eds.)

On behalf of the IAU fee forty eight "High power Astrophysics" a distinct consultation on "CNO Isotopes in Astrophysics" used to be held on the basic meeting of IAU in Grenoble on August 30, 1976. This subject was once selected because it has lately incorporated many interesting advancements in quite a few domain names of physics and astrophysics resembling for example meteoritical stories, radioastronomy measurements of the interstellar fuel, new determinations of nuclear reactions cross-sections and fractionation procedures. The papers of this quantity are the written types of the talks that have been offered in this consultation and canopy the newest observations and theoretical advancements re­ garding this fast-growing box. allow me thank first Professor Martin Rees (Institute of Astronomy at Cambridge) the chairman of IAU fee forty eight, who has backed this specified consultation and made it attainable. i'm indebted to the authors of the papers for his or her contributions and the entire paintings they've got installed the wonderful presentation of the fabric. lowe designated due to Professor William A. Fowler (Kellogg Laboratory at Cal tech) who has beautifully chaired this consultation and made it very intriguing and full of life, to Professor Beatrice M. Tinsley (Yale collage) who accep­ ted the tough activity to finish and sGmmarize on this sort of burning and relocating subject, and to Dr James Lequeux for his valuable assist in the version of a number of contributions. ultimately, the variation of this e-book wouldn't have been attainable with­ out the expert and beneficiant relief of pass over Jeannette Caro.

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Additional resources for CNO Isotopes in Astrophysics: Proceedings of a Special IAU Session Held on August 30, 1976, in Grenoble, France

Example text

The spectral interval covered by the 2048 channels of the scan was roughly AA3100-5200A. All spectra were normalized by the observation of blue standard stars of known energy distribution (Hayes 1970, Stone 1974), and fluxes FA were C AND N ABUNDANCES IN STARS OF THE METAL POOR GLOBULAR CLUSTER M92 35 derived across the entire spectral range. Six of the seven field giants studied by Sneden (1974) were also observed with the same equipment and were used as control over the method of analysis •. Further observational details and an extensive description of the photometric accuracy will be given in a forthcoming paper to be published in the Astrophysical Journal.

Identical to the metal content of M92 stars (cf. Butler 1975, and references therein). 8) lie nearest the SGB and M92. According to Sneden, these objects have [i] ~ r~] ~ [~]. The other five giants have carbon deficient and nitrogen overabundant, presumably as a result of the mixing of CNOprocessed material into the external convection zone (Sneden 1974). These stars have lower surface gravities, therefore lie higher in the color-magnitude diagram, and thus are compatible with the view that they are representative of a later evolutionary stage than the stars with normal C and N.

The convective zone was not large enough to produce a significant enhancement of the envelope. Nevertheless, white dwarfs with lower masses develope larger convective zones (Fontaine and Van Horn, 1976) and accretion onto these stars should result in a larger number of carbon nuclei in the envelope. , 1977). We found t~at in models with low envelope mass (~10~, the expansion of the envelope during the rise to peak temperature ca~sed the outer edge of the core to expand and cool. The outermost zones of the core expanded more rapidly and quickly became convective.

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