Implications of the new globular-cluster metal-abundance scale for the helium abundance in the Galactic halo

Details Implications of the new globular-cluster metal-abundance scale for the helium abundance in the Galactic halo Implications of the new globular-cluster metal-abundance scale for the helium abundance in the Galactic halo

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...242l...5d&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 242, Nov. 15, 1980, p. L5-L7.

Other

10

Abundance, Galactic Evolution, Globular Clusters, Helium, Astronomical Catalogs, Halos, Metals, Star Clusters

Scientific paper

In the adoption of the new abundance scale for globular clusters (Cohen, 1980; Pilachowski et al, 1980) a difficulty in fitting main sequences of 47 Tucanae and other well-studied globular clusters, like M 3, M 5, and M 13 is pointed out. In order to circumvent this problem, a substantial difference in helium abundance must be invoked. Such differences can also cause the very faint turnoff magnitudes found recently by Alcaino and Liller (1980) for NGC 6397 and by Cannon (1974) for Omega Centauri, without the need to assign excessive ages to these clusters. Other consequences of this helium-abundance variation are discussed.

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