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A new method to simulate long-term evolution of stars near a massive Black Hole

Published online by Cambridge University Press:  11 March 2020

Y. Funato Open the ORCID record for Y. Funato [Opens in a new window]
Y. Funato*
Affiliation:
General Systems Studies,Graduate Division of International and Interdisciplinary Studies, University of Tokyo, 3-8-1 Komaba Meguro-ku Tokyo153-8902Japan email: [email protected]
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Abstract

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N-body simulation is the necessary tool to investigate the evolution of star clusters. It is important to develop a time integration method which guarantees the appropriate accuracy and calculation cost.

Here we present a new simple method for long term simulation of stars around a massive black hole in stellar systems. Usually the time integration orbits of stars revolving a massive black hole requires much simulation time. We introduce a time transformation which is a kind of ”inverse KS regularization” of time. Using our method, the integration of the long term evolution near a black hole (BH) becomes easier, especially applied to relatively large star clusters and the Galactic Center.

Keywords

methods: numericalgalaxies: evolutiongalaxies: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 434 - 437
Copyright
© International Astronomical Union 2020

References

Murray & Dermott 1999, Solar System Dynamics, (Cambridge University Press)Google Scholar