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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

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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