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Possible Characteristics of Supernova Induced Enrichment of Globular Clusters

Published online by Cambridge University Press:  04 August 2017

Graeme H. Smith
Graeme H. Smith*
Affiliation:
Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 U.S.A.

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Within globular clusters, stars of similar temperatures and gravities commonly exhibit differences in the strength of the λ3883 CN band, the distribution of which is often bimodal. An archetype example of this phenomenon is NGC 6752 (Norris et al. 1981). As documented by Da Costa and Cottrell (1980), and Norris et al. (1981), the CN-rich giants in this cluster possess enhancements in nitrogen abundance by factors of 7–8 relative to the CN-poor giants. This may indicate that chemical enrichment of proto-cluster gas clouds took place as a result of the activity of massive stars, which manufactured nitrogen within their interiors and ejected it into the cluster gas while low mass stars were forming. The aim of this paper is to investigate whether the properties of NGC 6752 mentioned above might be consistent with supernova enrichment. Both the free and adiabatic expansion phases of supernova shells (Spitzer 1968) will be discussed in this context.

Type
May 29: Observations of Globular Clusters
Information
Symposium - International Astronomical Union , Volume 113: Dynamic of Stars Clusters , 1985 , pp. 105 - 108
Copyright
Copyright © Reidel 1985 

References

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