  The morphological distribution of primordial density peaks is assessed.
Previous determinations, those of Peacock & Heavens (1985) and those of Bardeen
et al (1986) have contradictory concluded that there exist a tendency towards
prolate or towards oblate shapes, respectively. By using two methods, the
Hessian and the inertia tensor momenta we have performed numerical
determinations of the triaxiality of density perturbations in Gaussian random
fields with power law spectra. We show that there is no present any tendency of
shapes, and that the triaxiality distribution is independent of the spectral
index. Moreover, it is shown that the results of Peacock and Heavens are
compatible with our determinations. These results are in complete agreement
with current triaxial distributions inferred for galaxies and clusters both,
from observations and from numerical simulations.
