  We present preliminary results of our investigation into the influence of
shear fields on the evolution of galactic scale fluctuations in a primordial
Gaussian random density field. Specifically, we study how the matter associated
with a galaxy-scale peak evolves, to determine whether the shear can affect the
peak's ability to form a virialized structure. We find that the evolution of
the mass distribution in the immediate surroundings of $\geq 1\sigma$ initial
density peaks is sensitive to the nature and magnitude of the shear. Its final
fate and configuration spans a plethora of possibilities, ranging from
accretion onto the peak to complete disruption. On the other hand, the mass
defining the peak itself always tends to form a virialized object, though a
given galaxy-scale peak need not necessarily form only one halo. Furthermore,
galaxy-size halos need not necessarily be associated with initial galaxy-scale
density peaks. Under certain conditions, the shear field is capable of breaking
up a single primordial peak into two (and perhaps, more) distinct halos, or of
promoting the growth of smaller-scale peaks into galaxy-size halos.
