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The Evolution of the Integrated Colors of Globular Clusters and Elliptical Galaxies

Published online by Cambridge University Press:  14 August 2015

R.B. Ciardullo  and
P. Demarque
R.B. Ciardullo
Affiliation:
Yale University Observatory
P. Demarque
Affiliation:
Yale University Observatory

Extract

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The purpose of this paper is to show the first results of a program designed to construct population models of stellar systems on the basis of theoretical data of stellar evolution. Synthetic HR diagrams were obtained using the isochrones and luminosity functions of Ciardullo and Demarque (1977). This last work is based on the stellar models of the Yale - IBM research group (Mengel, Sweigart, Demarque and Gross 1978; Sweigart and Gross 1976; 1978). The conversion from the theoretical HR diagram to observable parameters is made with the help of theoretical model stellar atmospheres principally due to Kurucz (1976), Relyea (1976) and Bell and Gustafsson (1975). The program provides a synthetic C-M diagram and integrated properties for the system given the following parameters: the chemical composition in terms of the (Y,Z) pair, the age, the total number of stars, the initial mass function (IMF) and the law of mass loss from stars in the system. In this brief paper, we shall concentrate on the integrated properties of theoretical star clusters and then remark on some interesting consequences for the color evolution of elliptical galaxies.

Type
Part VII: Theoretical Papers and Summary
Information
Symposium - International Astronomical Union , Volume 80: The HR Diagram , 1978 , pp. 345 - 348
Copyright
Copyright © Reidel 1978 

References

Bell, R.A. and Gustafsson, B. (1975). In Multicolor Photometry and the Theoretical HR Diagram, Philip, A.G.D. and Hayes, D.S., eds., Dudley Obs. Report No. 9, p. 319.Google Scholar
Ciardullo, R.B. and Demarque, P. (1977). Trans. Yale Univ. Obs. Vol. 33, 34, 35.Google Scholar
Crane, P. (1975). Astrophys. J. Letters 198, L9.CrossRefGoogle Scholar
Demarque, P. and McClure, R.D. (1977a). Astrophys. J. 213, 716.Google Scholar
Demarque, P. and McClure, R.D. (1977b). Yale Conf. on The Evolution of Galaxies and Stellar Populations, Tinsley, B.M. and Larson, R.B., eds., Yale Univ. Obs., New Haven, p. 199.Google Scholar
Fusi-Pecci, F. and Renzini, A. (1975). Astron. Astrophys. 39, 413.Google Scholar
Heasley, J.N. and Mengel, J.G. (1972). Observatory 92, 93.Google Scholar
Hodge, P.W. (1961). Astron. J. 66, 83.Google Scholar
Kurucz, R.L. (1976). unpublished.Google Scholar
Mengel, J.G., Sweigart, A.V., Demarque, P. and Gross, P.G. (1978). to be published.Google Scholar
Oke, J.B. and Wilkinson, A. (1977). to be published.Google Scholar
Prather, M.J. (1976). , Yale University.Google Scholar
Racine, R. (1973). Astron. J. 78, 180.CrossRefGoogle Scholar
Racine, R. (1975). Astron. J. 80, 1031.CrossRefGoogle Scholar
Relyea, L. (1976). , SUNY Albany.Google Scholar
Salpeter, E.E. (1955). Astrophys. J. 121, 161.Google Scholar
Sweigart, A.V. and Gross, P.G. (1976). Astrophys. J. Suppl. 32, 367.CrossRefGoogle Scholar
Sweigart, A.V. and Gross, P.G. (1978). to be published.Google Scholar
Tinsley, B.M. (1977). to be published.Google Scholar
Tinsley, B.M. and Gunn, J.E. (1976). Astrophys. J. 203, 53.Google Scholar
van den Bergh, S. (1969). Astrophys. J. Suppl. 19, 145.Google Scholar