Abundances in metal-poor stars. II - The anomalous globular cluster Omega Centauri

Details Abundances in metal-poor stars. II - The anomalous globular cluster Omega Centauri Abundances in metal-poor stars. II - The anomalous globular cluster Omega Centauri

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...115..336g&link_type=abstract

Astronomy and Astrophysics, vol. 115, no. 2, Nov. 1982, p. 336-346. Research supported by the Consiglio Nazionale delle Ricerch

Astronomy and Astrophysics

Astronomy

45

Abundance, Globular Clusters, Late Stars, Metallic Stars, Calcium, Chemical Composition, Infrared Astronomy, Iron, Magnesium, Nuclear Fusion, Peculiar Stars, Silicon, Sodium, Tables (Data)

Scientific paper

An analysis of the chemical composition of eight red giants in the anomalous globular cluster co Centauri is presented. The inhomogeneity in the cluster chemical composition is confirmed, with iron abundances ranging from [Fe/H] = - 1.9 to [Fe/H] = - 1.3, the range being about three times the observational error of a single observation. All the observed elements show variations in abundance from star to star. The ranges of abundance for Na, Mg, Ca, and Si are considerably wider than for Fe, suggesting an enrichment process which favoured light elements with respect to heavier ones. In this respect the metal enrichment history for ω Centauri seems different from the general process for the galactic medium.
A tentative analysis for the (mild) CH star RGO 70 gives [Fe/H] = -1.9, putting this star into the group of the metal-poor ones within the cluster; s-element overabundances are suggested for star ROA 70, ROA 40 and ROA 219. A mixing origin for the anomalous abundances in these stars seems likely.
The iron abundances from high dispersion spectra correlates within the observational errors with the R(V- K) index defined by Persson et al. (1980); the w Centauri giants are on the mean bluer than indicated by their iron abundances as the M 13 and NGC 3201 ones.

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