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Regular and chaotic orbits in a self-consistent triaxial stellar system with slow figure rotation

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Abstract

We created a self-consistent triaxial stellar system through the cold disipationless collapse of 100,000 particles whose evolution was followed with a multipolar code. The resulting system rotates slowly even though its total angular momentum is zero, i.e., it offers an example of figure rotation. The potential of the system was subsequently approximated with interpolating formulae yielding a smooth potential stationary in the rotating frame. The Lyapunov exponents could then be computed for a randomly selected sample of 3,472 of the bodies that make up the system, allowing the recognition of regular and partially and fully chaotic orbits. The regular orbits were Fourier analyzed and classified using their locations on the frequency map. A comparison with a similar non-rotating model showed that the fraction of chaotic orbits is slightly but significantly enhanced in the rotating model; alternatively, there are no significant differences between the corresponding fractions neither of partially and fully chaotic orbits nor of long axis tubes, short axis tubes, boxes and boxlets among the regular orbits. This is a reasonable result because the rotation causes a breaking of the symmetry that may increase chaotic effects, but the rotation velocity is probably too small to produce any other significant differences. The increase in the fraction of chaotic orbits in the rotating system seems to be due mainly to the effect of the Coriolis force, rather than the centrifugal force, in good agreement with the results of other investigations.

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  1. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Instituto de Astrofísica La Plata (UNLP–CONICET), 1900, La Plata, Argentina

    J. C. Muzzio

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  1. J. C. Muzzio
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Correspondence to J. C. Muzzio.

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Muzzio, J.C. Regular and chaotic orbits in a self-consistent triaxial stellar system with slow figure rotation. Celestial Mech Dyn Astr 96, 85–97 (2006). https://doi.org/10.1007/s10569-006-9036-7

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  • DOI: https://doi.org/10.1007/s10569-006-9036-7

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