Self-consistent Triaxial Galaxies With Central Density Cusps
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**Session 25 -- Ellipticals and Dark Matter**
*Oral presentation, Monday, 9, 1995, 10:00am - 11:30am*

## [25.02] Self-consistent Triaxial Galaxies With Central Density Cusps

*T. Fridman, D. Merritt (Rutgers University)*

We present the first self-consistent models of triaxial galaxies
with central density cusps. The mass distribution is the triaxial
generalization of the spherical ``eta'' models, $\rho \propto
m^{\eta-3}(1+m)^{-1- \eta }$, $ m^{2} =\frac {x^{2}} {a^{2}} + \frac
{y^{2}} {b^{2}}+ \frac {z^{2}} {c^{2}} $. The eta models
look similar to a de Vaucouleurs profile in projection
but have a central cusp with a power-law slope that can be adjusted from
$0$ to $-2$. Here we present results for $\eta =1$, i.e. $\rho
\propto r^{-2}$ near the center, similar to the observed luminosity
density in M32. Most of the box orbits are unstable owing to the
central singularity; they are replaced by stochastic orbits, which
evolve strongly over a timescale of a few crossing times, and by some
regular orbits associated with resonances. We discuss the constraints
imposed by stochasticity on the shapes of triaxial models, and the
likely importance of stochastic orbits in causing a slow evolution of
elliptical galaxies.

**Monday
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