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Cluster CMDs from N-body Simulations: Stellar and Binary Evolution on GRAPE

Published online by Cambridge University Press:  26 May 2016

Jarrod R. Hurley
Jarrod R. Hurley*
Affiliation:
American Museum of Natural History, Department of Astrophysics, Central Park West at 79th Street, New York, NY 10024, USA

Abstract

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The Colour-Magnitude diagram (CMD) is an important observational tool for use in the study of star clusters. Thus it is important to include a consistent treatment of stellar and binary evolution in N-body codes to allow the generation and interaction of the full range of stellar populations. In this way realistic cluster models can be compared with observed cluster populations via the respective CMDs. Preliminary results of such an approach using the Aarseth NBODY4 code on the GRAPE-6 are presented here. In particular, by using a stellar evolution algorithm that includes metallicity as a free parameter, the stellar populations of clusters at various stages of evolution can be studied. Interesting formation cases directly influenced by the cluster environment are highlighted for various stellar sub-populations.

Type
Stellar Dynamics and Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 208: Astrophysical Supercomputing using Particle Simulations , 2003 , pp. 113 - 122
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Aarseth, S.J. 1999, PASP, 111, 1333 Google Scholar
Bailyn, C.D. 1995, ARA&A, 33, 133 Google Scholar
D'Antona, F., Vietri, M., & Pesce, E. 1995, MNRAS, 272, 730 Google Scholar
D'Cruz, N.L., Dorman, B., Rood, R.T., & O'Connell, R.W. 1996, ApJ, 466, 359 Google Scholar
Ferraro, F.R., Clementini, G., Fusi Pecci, F., Buonanno, R., & Alcaino, G. 1990, A&AS, 84, 59 Google Scholar
Ferraro, F.R., Fusi Pecci, F., Cacciari, C., Corsi, C., Buonanno, R., Fahlman, G.G., & Richer, H.B. 1993, AJ, 106, 2324 CrossRefGoogle Scholar
Guhathakurta, P., Webster, Z.T., Yanny, B., Schneider, D.P., & Bahcall, J.N. 1998, AJ, 116, 1757 Google Scholar
Hurley, J.R., Pols, O.R., & Tout, C.A. 2000, MNRAS, 315, 543 CrossRefGoogle Scholar
Hurley, J.R., Tout, C.A., Aarseth, S.J., & Pols, O.R. 2001, MNRAS, 323, 630 Google Scholar
Hurley, J.R., Tout, C.A., & Pols, O.R. 2001, MNRAS, accepted Google Scholar
Hurley, J.R., & Shara, M.M. 2001, ApJ, accepted Google Scholar
Iben, I. Jr. 1990, ApJ, 353, 215 CrossRefGoogle Scholar
Kurucz, R.L. 1992, in Barbuy, B., Renzini, A., eds. Proc. IAU Symp. 149, The Stellar Populations of Galaxies. (Kluwer: Dordrecht) Vol. 7, p. 225 CrossRefGoogle Scholar
Leonard, P.J.T. 1996, ApJ, 470, 521 Google Scholar
Rich, R.M., et al. 1997, ApJ, 484, L25 Google Scholar
Soker, N., & Harpaz, A. 2000, MNRAS, 317, 861 Google Scholar
Testa, V., Corsi, C.E., Andreuzzi, G., Iannicola, G., Marconi, G., Piersimoni, A.-M., & Buonanno, R. 2001, AJ, 121, 916 Google Scholar