Models of cuspy triaxial stellar systems - IV. Rotating systems

D. D. CARPINTERO; J. C. MUZZIO

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

WILEY-BLACKWELL PUBLISHING, INC

Lugar: Londres; Año: 2016 vol. 459 p. 1082 - 1096

0035-8711

We built two self--consistent models of triaxial, cuspy, rotating stellarsystems adding rotation to non-rotating models presented in previous papers ofthis series. The final angular velocity of the material is not constant andvaries with the distance to the center and with the height over the equator ofthe systems, but the figure rotation is very uniform in both cases. Even thoughthe addition of rotation to the models modifies their original semiaxes ratios,the final rotating models are considerably flattened and triaxial. An analysisof the orbital content of the models shows that about two thirds of their orbitsare chaotic yet the models are very stable over intervals of the order of one Hubble time. The bulk of regular orbits are short axis tubes, while long axis tubes are replaced by tubes whose axes lie on the short--long axes plane, but do not coincide with the major axis. Other types of regular orbits that do not appear in non--rotating systems, like horseshoes and orbits that cross themselves, are also found in the present models. Finally, our frequency maps show empty regions where studies of orbits on fixed potentials found orbits, a likely consequence of the self--consistency of our models that excludes them.