Nitrogen variations on the main sequence of 47 Tucanae - Implications from stellar structure theory

Details Nitrogen variations on the main sequence of 47 Tucanae - Implications from stellar structure theory Nitrogen variations on the main sequence of 47 Tucanae - Implications from stellar structure theory

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259..193d&link_type=abstract

Astrophysical Journal, Part 1, vol. 259, Aug. 1, 1982, p. 193-197.

Astronomy and Astrophysics

Astrophysics

39

Abundance, Globular Clusters, Main Sequence Stars, Nitrogen, Stellar Evolution, Stellar Structure, Carbon, Giant Stars, Helium, Oxygen, Sodium

Scientific paper

We present evolutionary calculations of a 0.9 Msun metal-poor star in which the outer layers are artificially mixed throughout the main-sequence lifetime. For the case where the mixed region contains 85% of the mass of the star, evolution toward the subgiant branch is relatively unaffected but no significant enhancement of the surface nitrogen abundance occurs. Alternatively, for the case of deeper mixing, significant surface nitrogen enhancements are produced but the star evolves as a blue straggler and does not become a red giant in a normal way. Thus the observations of large nitrogen abundance variations among main-sequence stars andgiants in the globular cluster 47 Tuc are unlikely to be the result of deep envelope mixing on the main sequence. Mixing at an advanced phase of evolution and mass transfer in close binaries also seem unlikely. We conclude therefore that the most plausible explanation of the observed variations is that they are primordial in origin, that is, they reflect the presence of nitrogen abundance inhomogeneities in the protocluster gas cloud.

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