Globular cluster colour-magnitude diagrams - Possible evidence for helium abundance variations

Details Globular cluster colour-magnitude diagrams - Possible evidence for helium abundance variations Globular cluster colour-magnitude diagrams - Possible evidence for helium abundance variations

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983prhe.work..223c&link_type=abstract

IN: ESO Workshop on Primordial Helium, Garching, West Germany, February 2, 3, 1983, Proceedings (A83-50030 24-90). Garching, Wes

Physics

2

Abundance, Globular Clusters, Helium, Stellar Evolution, Hertzsprung-Russell Diagram, Horizontal Branch Stars, Main Sequence Stars, Stellar Magnitude

Scientific paper

The difference in magnitude between the horizontal branch and the main sequence turn-off point in the cluster color-magnitude (CM) diagram is used to study helium abundance variations in globular clusters. CM diagrams are obtained for the clusters Omega Centauri, NGC 6397, and NGC 288, for which the delta Mv are found to be about 3.8, 3.7, and 3.5, respectively. The RR Lyrae period shift in Omega Cen supports the finding that the horizontal branch in that cluster is unusually bright for its metallicity; if this is due to an increase in helium abundance then that abundance is about 0.05 larger in Omega Cen than in M5 and M3. NGC 288 appears to be neither very old nor overabundant in helium, although it remains a good example of a 'second parameter' cluster in that it combines a purely horizontal blue branch with relatively high metallicity.

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