Abundances in metal-poor stars. I - The globular clusters NGC 2808, NGC 3201, NGC 6397, and M 22

Details Abundances in metal-poor stars. I - The globular clusters NGC 2808, NGC 3201, NGC 6397, and M 22 Abundances in metal-poor stars. I - The globular clusters NGC 2808, NGC 3201, NGC 6397, and M 22

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...115..171g&link_type=abstract

Astronomy and Astrophysics, vol. 115, no. 1, Nov. 1982, p. 171-184. Research supported by the Consiglio Nazionale delle Ricerch

Astronomy and Astrophysics

Astrophysics

56

Abundance, Giant Stars, Globular Clusters, Late Stars, Metallic Stars, Stellar Spectra, Atmospheric Models, Line Spectra, Radial Velocity, Spectrum Analysis, Tables (Data)

Scientific paper

Abundances are derived for giant stars in the globular clusters NGC 2808, NGC 3201, NGC 6397, and M 22 by means of echelle high dispersion spectra and a model atmosphere analysis. The data confirm the globular cluster metallicity scale found by means of previous high dispersion study. NGC 2808 is a metal rich globular cluster (Fe/H = -1.1); thus the blue part of the discontinuous horizontal branch is anomalous. The metal abundance of NGC 3201 is high. The couple of cluster NGC 3201-47 Tucanae shows clear analogy with the M 13-M 3 couple. It is suggested that a second parameter might affect the giant branch morphology. It might be correlated with the second parameter affecting the horizontal branch. There are no indications of inhomogeneities in M 22 for any element, Na included. There are no obvious differences in composition between metal rich globular clusters and metal-poor galactic clusters.

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