Orbital stability in rotating triaxial stellar systems

Details Orbital stability in rotating triaxial stellar systems Orbital stability in rotating triaxial stellar systems

Nov 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...206..269m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 206, no. 2, Nov. 1988, p. 269-278. Research supported by SNSF.

Statistics

Computation

21

Computational Astrophysics, Elliptical Galaxies, Galactic Rotation, Orbital Mechanics, Stellar Systems, Axes Of Rotation, Branching (Mathematics), Degrees Of Freedom, Density Distribution, Hamiltonian Functions

Scientific paper

Simple periodic orbits in simple triaxial mass models with different axial ratios are investigated for a variety of rotation speeds. Special attention is given to Ferrers' ellipsoids, and logarithmic potentials are considered for comparison. In all models, the equatorial retrograde orbit family exists for all values of the Hamiltonian, but the size of its instability strip depends on the geometry and on the rotation of the figure. Equatorial direct orbits exist for a limited range of the Hamiltonian. The connection of orbits tipped with respect to the (y,z) and (x,z) planes with the equatorial retrograde family and the z-axis family is clarified. When the rotation frequency Omega(p) increases, the sequence of bifurcation of the latter family is modified. Beyond some critical value it becomes complexly unstable, and the stable anomalous orbit no longer bifurcates from it. The constraints inferred from these findings for the construction of self-gravitating equilibrium models are considered.

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