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Title:
On time-dependent orbital complexity in gravitational N-body simulations
Authors:
Faber, N. T.; Boily, C. M.; Portegies Zwart, S.
Affiliation:
AA(Observatoire Astronomique, Université de Strasbourg and CNRS UMR 7550, 11 rue de l'Université, 67000 Strasbourg, France; Sterrenkundig Instituut `Anton Pannekoek', University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, the Netherlands; Section Computational Science, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, the Netherlands), AB(Observatoire Astronomique, Université de Strasbourg and CNRS UMR 7550, 11 rue de l'Université, 67000 Strasbourg, France), AC(Sterrenkundig Instituut `Anton Pannekoek', University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, the Netherlands; Section Computational Science, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, the Netherlands)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 386, Issue 1, pp. 425-439. (MNRAS Homepage)
Publication Date:
05/2008
Origin:
MNRAS
MNRAS Keywords:
methods: N-body simulations , methods: numerical , stars: kinematics
DOI:
10.1111/j.1365-2966.2008.13041.x
Bibliographic Code:
2008MNRAS.386..425F

Abstract

We implement an efficient method to quantify time-dependent orbital complexity in gravitational N-body simulations. The technique, which we name DWaTIM, is based on a discrete wavelet transform of velocity orbital time-series. The wavelet power spectrum is used to measure trends in complexity continuously in time. We apply the method to the test cases N = 3 Pythagorean configuration and a perturbed N = 5 Caledonian configuration. The method recovers the well-known time-dependent complexity of the dynamics in these small-N problems. We then apply the technique to an equal-mass collisional N = 256 body simulation run through core-collapse. We find that a majority of stars evolve on relatively complex orbits up to the time when the first hard binary forms, whereas after core-collapse, less complex orbits are found on the whole as a result of expanding mass shells.
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