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N-body Simulations with Live Stellar Evolution

Published online by Cambridge University Press:  05 March 2013

Ross P. Church ,
Christopher A. Tout  and
Jarrod R. Hurley
Ross P. Church*
Affiliation:
Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Vic 3800, Australia Institute of Astronomy, The Observatories, Madingley Road, Cambridge CB3 0HA, UK
Christopher A. Tout
Affiliation:
Institute of Astronomy, The Observatories, Madingley Road, Cambridge CB3 0HA, UK
Jarrod R. Hurley
Affiliation:
Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Vic 3800, Australia Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Vic 3122, Australia
*
DCorresponding author. Email: ross.church@sci.monash.edu.au
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Abstract

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An N-body code containing live stellar evolution through combination of the software packages nbody6 and stars is presented. Operational details of the two codes are outlined and the changes that have been made to combine them discussed. We have computed the evolution of clusters of 104 stars using the combined code and we compare the results with those obtained using nbody6 and the synthetic stellar evolution code sse. We find that, providing the physics package within stars is set up correctly to match the parameters of the models used to construct sse, the results are very similar. This provides a good indication that the new code is working well. We also demonstrate how this physics can be changed simply in the new code with convective overshooting as an example. Similar changes in sse would require considerable reworking of the model fits. We conclude by outlining proposed future development of the code to include more complete models of single stars and binary star systems.

Keywords

stars: evolutionstars: mass-lossmethods: N-body simulationsmethods: numericalopen clusters and associations: general
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 26 , Issue 1 , 2009 , pp. 92 - 102
Copyright
Copyright © Astronomical Society of Australia 2009

References

Aarseth, S. J., 1999, PASP, 111, 1333 Google Scholar
Aarseth, S. J., 2003, Gravitational N-Body Simulations (Cambridge University Press)CrossRefGoogle Scholar
Ahmad, A. & Cohen, L., 1973, JCoPh, 12, 389 Google Scholar
Baumgardt, H., Makino, J., Hut, P., McMillan, S. & Portegies Zwart, S., 2003, ApJ, 589, L25 CrossRefGoogle Scholar
Eggleton, P. P., 1971, MNRAS, 151, 351 CrossRefGoogle Scholar
Eggleton, P. P., Faulkner, J. & Flannery, B. P., 1973, A&A, 23, 325 Google Scholar
Eggleton, P. P., Fitchett, M. J. & Tout, C. A., 1989, ApJ, 347, 998 CrossRefGoogle Scholar
Haselgrove, C. B. & Hoyle, F., 1956, MNRAS, 116, 515 CrossRefGoogle Scholar
Henyey, L. G., Forbes, J. E. & Gould, N. L., 1964, ApJ, 139, 306 CrossRefGoogle Scholar
Holmberg, E., 1941, ApJ, 94, 385 CrossRefGoogle Scholar
Hurley, J. R., Pols, O. R. & Tout, C. A., 2000, MNRAS, 315, 543 CrossRefGoogle Scholar
Hurley, J. R., Pols, O. R. & Tout, C. A., 2002, MNRAS, 329, 897 Google Scholar
Hurley, J. R., Pols, O. R., Aarseth, S. J. & Tout, C. A., 2005, MNRAS, 363, 293 CrossRefGoogle Scholar
Kroupa, P., Tout, C. A. & Gilmore, G., 1993, MNRAS, 262, 545 CrossRefGoogle Scholar
Kudritzki, R. P. & Reimers, D., 1978, A&A, 70, 227 Google Scholar
Kustaanheimo, P. & Stiefel, E., 1965, J. Reine Angew. Math., 218, 204 CrossRefGoogle Scholar
Makino, J. & Taiji, M., 1998, Scientific simulations with specialpurpose computers: The GRAPE systems (Chichester; Toronto: John Wiley & Sons)Google Scholar
Mikkola, S. & Aarseth, S. J., 1990, CeMDA, 47, 375 Google Scholar
Oort, J. H., 1927, BAN, 3, 275 Google Scholar
Pols, O. R., Tout, C. A., Eggleton, P. P. & Han, Z., 1995, MNRAS, 274, 964 CrossRefGoogle Scholar
Pols, O. R., Schroder, K.-P., Hurley, J. R., Tout, C. A. & Eggleton, P. P., 1998, MNRAS, 298, 525 CrossRefGoogle Scholar
Portegies Zwart, S. F., McMillan, S. L. W., Hut, P. & Makino, J., 2001, MNRAS, 321, 199 CrossRefGoogle Scholar
Schröder, K.-P., Pols, O. R. & Eggleton, P. P., 1997, MNRAS, 285, 696 Google Scholar
Sills, A. et al., 2003, NewA, 8, 605 CrossRefGoogle Scholar
Schwarzschild, M. & Härm, R., 1962, ApJ, 136, 158 Google Scholar
Shaviv, G. & Salpeter, E. E., 1973, ApJ, 184, 191 Google Scholar
Stancliffe, R. J., 2005, PhD Thesis, University of Cambridge Google Scholar
Stancliffe, R. J., Tout, C. A. & Pols, O. R., 2004, MNRAS, 352, 984 CrossRefGoogle Scholar
Vassiliadis, E. & Wood, P. R., 1993, ApJ, 413, 641 CrossRefGoogle Scholar