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Observed Variations in the Density Profiles of Star Clusters in the LMC

Published online by Cambridge University Press:  19 July 2016

M. Kontizas ,
D. Hatzidimitriou  and
M. Metaxa
M. Kontizas
Affiliation:
Laboratory of Astrophysics, University of Athens
D. Hatzidimitriou
Affiliation:
University of Edinburgh
M. Metaxa
Affiliation:
Laboratory of Astrophysics, University of Athens

Extract

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Several dynamical theories have been developed in order to approach the dynamical evolution of stellar systems and explain the observational data. The observed density profiles of the clusters can be a valuable source of information towards the understanding of their dynamical properties. King in a series of papers has connected the established theories with the observed profiles in clusters of our own Galaxy (King, 1962, 1966; etc.). Density profiles can be obtained by means of star counts and/or by means of photometric photometry. So far the observations for clusters in our Galaxy and the MCs appear to fit well the so called King models and provide information of their tidal radii, total masses and concentration parameters (Kontizas, 1984).

Type
Chapter VIII. Poster Papers on Cluster Systems in Nearby Galaxies
Information
Symposium - International Astronomical Union , Volume 126: The Harlow-Shapley Symposium on Globular Cluster Systems in Galaxies , 1988 , pp. 571 - 572
Copyright
Copyright © Kluwer 1988 

References

REFERENCES

Agekyan, T. A. and Belozerova, M. A. 1977 Soviet Astronomy 23, 4.Google Scholar
King, I. R. 1962 Astron. J. 67, 471.Google Scholar
King, I. R. 1966 Astron. J. 71, 64.Google Scholar
Kontizas, M. 1984 Astron. Astrophys. 131, 58.Google Scholar