Numerical Investigations of a New N-body Simulation Method
Author(s)
E. Vilkoviskij*
ABSTRACT
Numerical investigation of a new similarity method (the Aldar-Kose method) for N-body simulations is described. Using this method we have carried out numerical simulations for two tasks: 1) calculation of the temporal behavior of different physical parameters of active galactic nuclei (AGN) containing a super massive black hole (SMBH), an accretion disk, and a compact stellar cluster; 2) calculation of the stellar capture rate to the central SMBH without accretion disk. The calculations show good perspectives for applications of the similarity method to optimize the evolution model calculations of large stellar systems and of AGN.
Numerical investigation of a new similarity method (the Aldar-Kose method) for N-body simulations is described. Using this method we have carried out numerical simulations for two tasks: 1) calculation of the temporal behavior of different physical parameters of active galactic nuclei (AGN) containing a super massive black hole (SMBH), an accretion disk, and a compact stellar cluster; 2) calculation of the stellar capture rate to the central SMBH without accretion disk. The calculations show good perspectives for applications of the similarity method to optimize the evolution model calculations of large stellar systems and of AGN.
Cite this paper
E. Vilkoviskij, "Numerical Investigations of a New N-body Simulation Method," International Journal of Astronomy and Astrophysics, Vol. 2 No. 3, 2012, pp. 119-124. doi: 10.4236/ijaa.2012.23016.
E. Vilkoviskij, "Numerical Investigations of a New N-body Simulation Method," International Journal of Astronomy and Astrophysics, Vol. 2 No. 3, 2012, pp. 119-124. doi: 10.4236/ijaa.2012.23016.
References
[1] E. Vilkoviskij, “On the New Method of N-Body Simula-tions,” IJAA, 2012, in press. [2] E. Vilkoviskij and B. Czerny, “The Role of the Central Stellar Cluster in AGN,” Astronomy and Astrophysics, Vol. 387, No. 3, 2002, pp. 804-819.doi:10.1051/0004-6361:20020255 [3] J. Frank and M. Rees, “Effects of Massive Central Black Holes on Dense Stellar Systems”, Monthly Notices of the Royal Astronomical Society, Vol. 176, 1976, pp. 633-647 [4] M. Brockamp, H. Baumgardt and P. Kroupa, “Tidal Dis-ruption Rate of Stars by Supermassive Black Holes Ob-tained by Direct N-Body Simulations,” arXiv: 1108.2270v1, 2011. [5] S. Aarseth and D. Heggie, “Basic N-Body Modelling of the Evolution of Globular Clusters. I. Time Scaling,” arXiv: astro-ph /9805344V1, 1998. [6] S. Harfst, A. Gualandris, D. Merritt, R. Spurzem, S. P. Zwart and P. Berczik, “Performance Analysis of Direct N-Body Algorithms on Special-Purpose Supercomputers,” New Astronomy, Vol. 12, No. 5, 2007, pp. 357-377.doi:10.1016/j.newast.2006.11.003
[1] E. Vilkoviskij, “On the New Method of N-Body Simula-tions,” IJAA, 2012, in press. [2] E. Vilkoviskij and B. Czerny, “The Role of the Central Stellar Cluster in AGN,” Astronomy and Astrophysics, Vol. 387, No. 3, 2002, pp. 804-819.doi:10.1051/0004-6361:20020255 [3] J. Frank and M. Rees, “Effects of Massive Central Black Holes on Dense Stellar Systems”, Monthly Notices of the Royal Astronomical Society, Vol. 176, 1976, pp. 633-647 [4] M. Brockamp, H. Baumgardt and P. Kroupa, “Tidal Dis-ruption Rate of Stars by Supermassive Black Holes Ob-tained by Direct N-Body Simulations,” arXiv: 1108.2270v1, 2011. [5] S. Aarseth and D. Heggie, “Basic N-Body Modelling of the Evolution of Globular Clusters. I. Time Scaling,” arXiv: astro-ph /9805344V1, 1998. [6] S. Harfst, A. Gualandris, D. Merritt, R. Spurzem, S. P. Zwart and P. Berczik, “Performance Analysis of Direct N-Body Algorithms on Special-Purpose Supercomputers,” New Astronomy, Vol. 12, No. 5, 2007, pp. 357-377.doi:10.1016/j.newast.2006.11.003