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The Structure and Internal Kinematics of Open Clusters

Published online by Cambridge University Press:  04 August 2017

Robert D. Mathieu
Robert D. Mathieu*
Affiliation:
Center for Astrophysics, Cambridge, Massachusetts

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Open clusters provide an opportunity for observational study of several important facets of stellar dynamics which cannot easily be addressed in globular clusters for either fundamental or practical reasons. In particular, open clusters are case studies for:

  1. 1) The dynamics of small-N stellar systems. This aspect of open clusters has been excellently reviewed by King (1980), to which the reader is referred. The work of Retterer (1979) and Goodman (this volume) suggests that any differences in the velocity distributions of small-N systems as compared to large-N systems due to the increased importance of close stellar encounters will appear primarily in the high-energy tails of the distributions. This will be reflected in the structure of the cluster halos, where quality data are difficult to obtain. In order to guide observational study, more theoretical work is needed regarding the expected nature and magnitude of any observable deviations from large-N theory.

  2. 2) The effects of a large stellar-mass spectrum. While globular clusters probably also have a spectrum of masses spanning an order of magnitude or more, the extension of the mass spectrum to higher masses in open clusters permits the dynamical consequences of a mass spectrum to be more easily studied. In addition, many studies have pointed out the significance of stellar mass lośs in massive stars for the evolution of clusters (e.g., Terlevich 1983). However, as yet the theory regarding the effects of such mass loss has not provided unique observational predictions which might act as critical tests, so this important issue will not be discussed further here.

  3. 3) A spectrum of cluster ages. Open clusters span the complete spectrum of age from birth to dissolution. Except for the classic work of Wielen (1971 and this volume) in which he analyses the observed distribution of cluster ages, this feature of open clusters has been little exploited. Yet by mapping appropriate diagnostics with cluster age open clusters have the potential to provide empirical measures of the fundamental dynamical time-scales, e.g. the relaxation time, equipartition time and mixing time. Also, study of the very youngest clusters provides appropriate initial conditions for evolutionary models as well as insight into star- and cluster-formation processes.

  4. 4) The effect of the external environment. Open cluster halos are molded by the galactic tidal field. In addition, open clusters are subject to Impulsive encounters with clouds in the interstellar medium. The effects of these environmental influences can be examined in numerous ways, including detailed analyses of the structure of cluster halos and observations of the variation with radius of anisotropy in the cluster velocity distributions.

Type
Open Clusters
Information
Symposium - International Astronomical Union , Volume 113: Dynamic of Stars Clusters , 1985 , pp. 427 - 448
Copyright
Copyright © Reidel 1985 

References

Aarseth, S. J.: 1975, Dynamics of Stellar Systems (ed. Hayli, A.), p. 57 (Dordrecht: Reidel)CrossRefGoogle Scholar
Abt, H. A.: 1980, Ap. J. 241, 275.CrossRefGoogle Scholar
Abt, H. A. and Levy, S. G.: 1976, Ap. J. Supp., 30, 273.CrossRefGoogle Scholar
Bahcall, J.: 1984, Ap. J. 276, 169.CrossRefGoogle Scholar
Bettis, C.: 1977, Ap. J. 214, 106.CrossRefGoogle Scholar
Brosche, P. and Hoffmann, M.: 1979, Astrop. and Space Science, 63, 467.CrossRefGoogle Scholar
Burki, G.: 1978, Astron. and Ap. 62, 159.Google Scholar
Chiu, G. and van Altena, W.: 1981, Ap. J., 243, 827.CrossRefGoogle Scholar
Cudworth, K. M.: 1971, A. J., 76, 475.CrossRefGoogle Scholar
Cudworth, K. M.: 1976, A.J., 81, 519.CrossRefGoogle Scholar
Cudworth, K. M.: 1979, A. J., 84, 1312.CrossRefGoogle Scholar
Elmegreen, B. G.: 1983, M.N.R.A.S., 203, 1011.CrossRefGoogle Scholar
Gieseking, F. J.: 1981, Astron. and Ap., 99, 155.Google Scholar
Heggie, D. C.: 1975, Dynamics of Stellar Systems (ed. Hayli, A.), p. 73, (Dordrecht: Reidel).CrossRefGoogle Scholar
Herbst, W. and Miller, D. P.: A.J., 87, 1478.CrossRefGoogle Scholar
King, I. R.: 1980, Star Clusters (ed. Hesser, J.), p. 139, (Dordrecht: Reidel).CrossRefGoogle Scholar
Jones, B. J.: 1970, A.J. 75, 563.CrossRefGoogle Scholar
Jones, B. J.: 1971, A.J. 76, 470.CrossRefGoogle Scholar
Lada, C. J., Margulis, M. and Dearborn, D.: 1984, Ap. J., in press.Google Scholar
Mathieu, R. D.: 1983a, Ap. J. Letters, 267, L97.CrossRefGoogle Scholar
Mathieu, R. D.: 1983b, Ph.D. dissertation, Univ. Cal. Berkeley.Google Scholar
Mathieu, R. D.: 1984, Ap. J., 284, in press.CrossRefGoogle Scholar
Mathieu, R. D. and Latham, D. W.: 1985a, in preparation.Google Scholar
Mathieu, R. D. and Latham, D. W.: 1985b, in preparation.Google Scholar
Mathieu, R. D., Stefanik, R. P. and Latham, D. W.: 1985, in preparation.Google Scholar
Mayor, M. and Mermilliod, J.C.: 1983, Les Etoiles Binaires dans le Diagramme H. R. (eds. Florsch, A., Jaschek, C. and Jaschek, M.), p. 45, (Observatoire de Strasbourg).Google Scholar
McNamara, B. J., Pratt, N. M. and Sanders, W. L.: 1977, Astron. and Ap. Supp., 27, 117.Google Scholar
McNamara, B. J. and Sanders, W. L.: 1977, Astron. and Ap., 54, 569.Google Scholar
McNamara, B. J. and Sanders, W. L.: 1978, Astron. and Ap., 62, 259.Google Scholar
McNamara, B. J. and Sanders, W. L.: 1983, Astron. and Ap., 118, 361.Google Scholar
Oort, J. H.: 1979, Astron. and Ap., 78, 312.Google Scholar
Pels, G., Oort, J. H. and Pels-Kluyver, H. A. 1975, Astron. and Ap., 43, 243.Google Scholar
Retterer, J. M.: 1979, A. J. 84, 370.CrossRefGoogle Scholar
Sanders, W. L.: 1977, Astron. and Ap. Supp., 27, 89.Google Scholar
Spitzer, L. Jr. and Shull, J. M.: 1975, Ap. J. 201, 773.CrossRefGoogle Scholar
Terlevich, E.: 1983, Ph.D. dissertation, University of Cambridge.Google Scholar
Tonry, J. and Davis, M.: 1979, A. J., 84, 1511.CrossRefGoogle Scholar
Van Bueren, H. G.: 1952, Bull. Astron. Inst. Neth., 11, 385.Google Scholar
van den Bergh, S. and Sher, D.: 1960, Pub. David Dunlap Obs., 2, 203.Google Scholar
van Leeuwen, F.: 1980, Star Clusters (ed. Hesser, J.), p. 157, (Dordrecht: Reidel).CrossRefGoogle Scholar
van Leeuwen, F.: 1983, Ph.D. dissertation, Sterrewacht Leiden.Google Scholar
Vasilevskis, S., van Leeuwen, F., Nicholson, W. and Murray, C. A.: 1979, Astron. and Ap. Suppl, 37, 333.Google Scholar
Weilen, R.: 1971, Astron. and Ap., 13, 309.Google Scholar
Weilen, R.: 1975, Dynamics of Stellar Systems (ed. Hayli, A.), p. 119, (Dordrecht: Reidel).CrossRefGoogle Scholar