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Masses and Relaxation Times of Star Clusters in the SMC

Published online by Cambridge University Press:  04 August 2017

M. Kontizas  and
E. Kontizas
M. Kontizas
Affiliation:
University of Athens, Observatory of Athens
E. Kontizas
Affiliation:
University of Athens, Observatory of Athens

Abstract

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Plates taken with the 1.2m U.K. Schmidt Telescope and the 3.8 AAT Telescope have been used in order to derive the dynamical parameteres of 43 various clusters of the SMC by means of star counts. The clusters are divided into two main categories: (i) the disk, “blue” and “intermediate” in colour, young, mainly globulars and (ii) the halo, “red”, old globular clusters. The disk clusters have been found to be more massive and older than the galactic open clusters, whereas the halo clusters are at least 10 times less massive than the galactic globulars. The relaxation times of the disk clusters are larger than their evolutionary age while the observed density profiles always show evidence of well relaxed systems.

Type
Magellanic Cloud Clusters
Information
Symposium - International Astronomical Union , Volume 108: Structure and Evolution of the Magellanic Clouds , 1984 , pp. 25 - 26
Copyright
Copyright © Reidel 1984 

References

Freeman, K.C. (1974). ESO/SRC/CERN Conference on Research Programs for the New Large Telescopes, Geneva, May, 1974.Google Scholar
Geyer, E.H. Hopp, U. (1982). IAU Colloquium No. 68, 235.Google Scholar
King, I.R. (1962), Astron. J., 67, 471.Google Scholar
Kontizas, M., Danezis, E., Kontizas, E. (1982). Astron. & Astroph. Suppl. Ser. 49, 1.Google Scholar
Kontizas, E. and Kontizas, M. (1983). Astron. & Astroph. Suppl. Ser. 53, 143.Google Scholar