Comparative study between N-body and Fokker–Planck simulations for rotating star clusters – I. Equal-mass system
Corresponding Author
Eunhyeuk Kim
FPRD, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea
E-mail: [email protected]Search for more papers by this authorIlsang Yoon
FPRD, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea
Department of Astronomy, University of Massachusetts, Amherst, MA 01002, USA
Search for more papers by this authorHyung Mok Lee
FPRD, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea
Search for more papers by this authorRainer Spurzem
Astronomische Rechen-Institut, Zentr. Astron. Univ. Heidelberg (ZAH), Monchhofstrasse 12-14, 69120 Heidelberg, Germany
Search for more papers by this authorCorresponding Author
Eunhyeuk Kim
FPRD, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea
E-mail: [email protected]Search for more papers by this authorIlsang Yoon
FPRD, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea
Department of Astronomy, University of Massachusetts, Amherst, MA 01002, USA
Search for more papers by this authorHyung Mok Lee
FPRD, Department of Physics and Astronomy, Seoul National University, Seoul 151-742, Korea
Search for more papers by this authorRainer Spurzem
Astronomische Rechen-Institut, Zentr. Astron. Univ. Heidelberg (ZAH), Monchhofstrasse 12-14, 69120 Heidelberg, Germany
Search for more papers by this authorABSTRACT
We have carried out N-body simulations for rotating star clusters with equal mass and compared the results with Fokker–Planck models. These two different approaches are found to produce fairly similar results, although there are some differences with regard to the detailed aspects. We confirmed the acceleration of the core collapse of a cluster due to an initial non-zero angular momentum and found a similar evolutionary trend in the central density and velocity dispersion in both simulations. The degree of acceleration depends on the initial angular momentum. Angular momentum is being lost from the cluster due to the evaporation of stars with a large angular momentum on a relaxation time-scale.
REFERENCES
-
Aarseth S. J., 1999, PASP, 111, 1333
10.1086/316455 Google Scholar
- Ardi E., Mineshige S., Spurzem R., 2005, JKAS, 38, 207
- Baumgardt H., 2001, MNRAS, 325, 1323
- Berczik P., Merritt D., Spurzem R., Bischof H. P., 2006, ApJ, 642, 21
- Binney J., Tremaine S., 1987, Galactic Dynamics. Princeton Univ. Press, Princeton , NJ
- Boily C. M., 2000, in A. Lancon, C. M. Boily, eds, ASP Conf. Ser. Vol. 211, Massive Stellar Clusters. Astron. Soc. Pac., San Francisco , p. 190
- Boily C. M., Spurzem R., 2000, in A. Noels, P. Magain, D. Caro, E. Jehin, G. Parmetier, A. A. Thoul, eds, Proc. of the 35th Liege Intern. Astroph. Colloq. The Galactic Halo: From Globular Clusters to Field Stars, p. 607
- Cohn H., 1980, ApJ, 242, 765
- Drukier G. A., Fahlman G. G., Richer H. B., 1992, ApJ, 386, 106
- Einsel C., Spurzem R., 1999, MNRAS, 302, 81 (Paper I)
- Ernst A., Glaschke P., Fiestas J., Just A., Spurzem R., 2007, MNRAS, 377, 465
- Fiestas J., Spurzem R., Kim E., 2006, MNRAS, 373, 677
- Freitag M., Benz W., 2001, A&A, 375, 711
-
Freitag M.,
Rasio F. A.,
Baumgardt H., 2006, MNRAS, 368, 121
10.1111/j.1365-2966.2006.10095.x Google Scholar
- Fukushige T., Makino J., Kawai A., 2005, PASJ, 57, 1009
- Giersz M., 1998, MNRAS, 298, 1239
- Giersz M., Heggie D. C., 1994a, MNRAS, 268, 257
- Giersz M., Heggie D. C., 1994b, MNRAS, 270, 298
- Giersz M., Heggie D. C., 1997, MNRAS, 286, 709
- Giersz M., Spurzem R., 1994, MNRAS, 269, 241
- Goodman J., 1983, PhD thesis, Princeton Univ.
- Goodman J., 1987, ApJ, 313, 576
- Harfst S., Gualandris A., Merritt D., Spurzem R., Portegies Zwart S., Berczik P.2007, New Astron., 12, 357
- Hénon M. H., 1971, Ap&SS, 14, 151
- Iwasawa M., Funato Y., Makino J., 2006, ApJ, 651, 1059
- Joshi K. J., Rasio F. A., Portegies Zwart S., 2000, ApJ, 540, 969
- Khalisi E., Amaro-Seoane P., Spurzem R., 2007, MNRAS, 374, 703
- Kim E., 2003, PhD thesis, Seoul National Univ.
- Kim E., Einsel C., Lee H. M., Spurzem R., Lee M. G., 2002, MNRAS, 334, 310 (Paper II)
- Kim E., Lee H. M., Spurzem R., 2004, MNRAS, 351, 220 (Paper III)
- Kustaanheimo P., Stiefel E., 1965, J. Reine Angew. Math., 218, 204
- Lee H. M., Goodman J., 1995, ApJ, 443, 109L
- Lee H. M., Ostriker J. P., 1987, ApJ, 322, L123
- Lee K. H., Lee H. M., Sung H., 2006, MNRAS, 367, 646
- Lupton R. H., Gunn J. E., 1987, AJ, 93, 1106
-
Makino J.,
Fukushige T.,
Koga M.,
Namura K., 2003, PASJ, 55, 1163
10.1111/j.1365-2966.2007.11720.x Google Scholar
- Makino J., Funato Y., 2004, ApJ, 602, 93
- Makino J., Taiji M., 1998, Scientific Simulations with Special-Purpose Computers–the GRAPE Systems. Wiley VCH
- Mikkola S., Aarseth S. J., 1990, CeMDA, 47, 375
- Mikkola S., Aarseth S. J., 1993, CeMDA, 57, 439
- Mikkola S., Aarseth S. J., 1996, CeMDA, 64, 197
- Mikkola S., Aarseth S. J., 1998, New Astron., 3, 309
- Spitzer L. J., Hart M. H., 1971, ApJ, 166, 483
- Spitzer, L. Jr., Mathieu R. D., 1980, ApJ, 241, 618
- Spurzem R., Aarseth S. J., 1996, MNRAS, 282, 19S
- Spurzem R., Giersz M., Takahashi K., Ernst A., 2005, MNRAS, 364, 948
- Takahashi K., 1995, PASJ, 47, 561
- Takahashi K., 1996, PASJ, 48, 691
- Takahashi K., 1997, PASJ, 49, 547
- Takahashi K., Lee H. M., 2000, MNRAS, 316, 617
- Takahashi K., Portegies Zwart S. F., 1998, ApJ, 503, L49
- Takahashi K., Portegies Zwart S. F., 2000, ApJ, 535, 759
- Yim K., Lee H. M., 2002, JKAS, 35, 75Y
