Strong cyanogen stars - The result of binary coalescence?

Details Strong cyanogen stars - The result of binary coalescence? Strong cyanogen stars - The result of binary coalescence?

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...307..750c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 307, Aug. 15, 1986, p. 750-759. Research supported by the National Research

Astronomy and Astrophysics

Astrophysics

26

Binary Stars, Cosmochemistry, Cyanogen, Stellar Evolution, Abundance, Coalescing, Galactic Nuclei, Globular Clusters, Open Clusters, Stellar Composition

Scientific paper

Many close binary stars are expected to coalesce during or after the MS phase of the primary. Such mergers could lead to contamination of the surface layers of the remnant by material processed in the core of the secondary. Since this material is nitrogen-rich, these events could explain the origin of the CN-strong (CNS) stars in the field and open clusters. For this hypothesis to explain the cyanogen anomalies of globular-cluster stars, there would have to be a substantial frequency of binaries in these clusters, which has not been observed to date. It is suggested that such binaries might have been missed because dynamical effects have caused them to become hard, concentrated toward the centers of clusters, evolved to very low mass ratios, and perhaps already coalesced. Binary mergers would explain the dichotomy in CN strength and anticorrelation of carbon and nitrogen found in many clusters. In 47 Tuc, mergers would also account for CNS stars on the MS and subgiant branches, and for the central concentration of CNS giants.

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