Particle realizations with N=512000 were generated from distribution functions that fit the photometric and kinematic data of M32. We constructed equal-mass particle realizations, and also realizations with a mass spectrum to improve the central resolution. Models were studied for two representative inclinations, i=90 degrees (edge-on) and i=55 degrees, corresponding to intrinsic axial ratios of q=0.73 and q=0.55, respectively. The time evolution of the models was calculated with a `self-consistent field' code on a Cray T3D parallel supercomputer. We find both models to be dynamically stable. This implies that they provide a physically meaningful description of M32, and that the inclination of M32 (and hence its intrinsic flattening) cannot be strongly constrained through stability arguments.
Previous work on the stability of f(E,L_z) models has shown that the
bar-mode is the most common unstable mode for systems rounder than
q=0.3 (i.e., E7), and that the likelihood for this mode to be unstable
increases with flattening and rotation rate. The f(E,L_z) models
studied for M32 are not bar-unstable, and M32 has a higher rotation
rate than nearly all other elliptical galaxies. This suggests that
f(E,L_z) models constructed to fit data for real elliptical galaxies
will generally be stable, at least for systems rounder than q > 0.55,
and possibly for flatter systems as well.