Complex instability around the rotation axis of stellar systems. I - Galactic potentials

Details Complex instability around the rotation axis of stellar systems. I - Galactic potentials Complex instability around the rotation axis of stellar systems. I - Galactic potentials

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...173...81m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 173, no. 1, Feb. 1987, p. 81-85. Research supported by the Universite de Genev

Astronomy and Astrophysics

Astrophysics

29

Dynamic Stability, Galactic Rotation, Gravitational Fields, Orbit Perturbation, Stellar Systems, Hubble Diagram, Mass Distribution, Periodic Variations, Stochastic Processes

Scientific paper

The frequent instability of the radial periodic orbits along the rotation axis of bulges, spheroids and other rotating triaxial ellipsoids is numerically investigated in some realistic gravitational potentials. For many cases, especially in nearly axisymmetric systems, complex instability sets in as soon as some rotation takes place. In general the classical sequence of bifurcation stable to semi-unstable to unstable found by Heissler et al. (1982) evolves to the sequence stable to semi-unstable to stable to complex unstable, and finally to the sequence stable to complex unstable when the figure rotation omega p is increased. The critical values of omega p depends on the density axis ratio of the system. The addition of a concentrated mass in the core modifies this behavior in the sense that the maximum orbital amplitude at which the bifurcation stable to complex unstable occurs is lowered. The diffusion time of chaotic orbits, starting along the rotation axis rapidly becomes shorter than the Hubble time when the central mass makes all the z-axis orbits complex unstable.

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