Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998larm.confe.119g&link_type=abstract
"IX Latin American Regional IAU Meeting, "Focal Points in Latin American Astronomy", held in Tonantzintla, Mexico, Nov 9-13, 199
Astronomy and Astrophysics
Astronomy
Scientific paper
We study the stability of trajectories near the disk plane of galaxy models with a triaxial dark matter halo component, examining the effect of weak discreteness noise, rapidly rotating bar perturbations and weak dissipation on these trajectories. For a triaxial matter distribution we find that dissipation may lead to the formation of a central mass concentration, which in turn destabilises the trajectories of stars formed in the central region. The addition of rapidly rotating bar perturbations also dramatically increases the degree of instability. Thus, if bars can form in triaxial haloes, they are likely to be quickly destroyed, leaving behind a bulge-like structure (which may explain the absence of bars in surveys of high redshift galaxies). We are extending our analysis of triaxial models using a new numerical procedure for determining self-consistent density and potential pairs for such systems. This procedure uses a Monte Carlo integration technique to efficiently map out the initial positions and velocities of those orbits which have significant non-zero Liapunov exponents. The numerical algorithm is sufficiently fast to allow us to explore a wide region of parameter space - varying the triaxiality and mass of the halo, and the mass of the disk and central mass concentration - and thus to investigate the impact of chaotic trajectories on the stability of the disk in triaxial systems.
El-Zant Amr A.
Gonzalez Alejandro
Hendry Martin
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