  A database on shape evolution of direct N-body models formed out of cold,
dissipationless collapse is generated using GRAPE and HARP special purpose
computers. Such models are important to understand the formation of elliptical
galaxies.
  Three dynamically distinct phases of shape evolution were found, first a fast
dynamical collapse which gives rise to the radial orbit instability (ROI) and
generates at its end the maximal triaxiality of the system. Subsequently, two
phases of violent and two-body shape relaxation occur, which drive the system
first towards axisymmetry, finally to spherical symmetry (the final state,
however, is still much more concentrated than the initial model).
  In a sequence of models the influence of numerical and physical parameters,
like particle number, softening, initial virial ratio, timestep choice,
different N-body codes, are examined. We find that an improper combination of
softening and particle number can produce erroneous results. Selected models
were evolved on the secular timescale until they became spherically symmetric
again. The secular shape relaxation time scale is shown to agree very well with
the two-body relaxation time, if softening is properly taken into account for
the latter. Finally, we argue, that the intermediate phase of violent shape
relaxation after collapse is induced by strong core oscillations in the centre,
which cause potential fluctuations, dampening out the triaxiality.
