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Observations of CO and OI in Stars in Globular Clusters

Published online by Cambridge University Press:  14 August 2015

George Wallerstein  and
Catherine Pilachowski
George Wallerstein
Affiliation:
University of Washington, Seattle
Catherine Pilachowski
Affiliation:
University of Washington, Seattle

Extract

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During the past decade it has been evident that the morphologies of globular cluster color-magnitude diagrams cannot be described by only two parameters, age and metal abundance (Sandage and Wildey 1967, Hartwick 1968). The third parameter is unlikely to be helium because a normal helium abundance is needed to explain the pulsation of RR Lyrae stars (Deupree 1977) and because the helium abundance of the planetary nebula in the metal-poor cluster M15 is normal (O'Dell et al. 1964).

Type
Part IV: HR Diagrams, Clusters
Information
Symposium - International Astronomical Union , Volume 80: The HR Diagram , 1978 , pp. 173 - 176
Copyright
Copyright © Reidel 1978 

References

Baldwin, J.R., Frogel, J.A. and Persson, S.E. (1973). Astrophys. J. 184, 427.Google Scholar
Deupree, R.G. (1977). Astrophys. J. 214, 502.Google Scholar
Hartwick, F.D.A. (1968). Astrophys. J. 154, 475.Google Scholar
Heifer, H.L. and Wallerstein, G. (1968). Astrophys. J. Suppl. 16, 1.Google Scholar
O'Dell, C.R., Peimbert, M. and Kinman, T.D. (1964). Astrophys. J. 140, 119.Google Scholar
Sandage, A.R. and Wildey, R.L. (1967). Astrophys. J. 150, 469.Google Scholar