  We analyze the spatial anisotropy and the velocity anisotropy in a set of
mock stellar halos from the Aquarius simulations. The spatial anisotropy in
each mock stellar halo rises progressively with the increasing distance from
the halo centre, eventually reaching a maximum near the periphery. Excluding
the bound satellites leads to a significant reduction of the spatial anisotropy
in each halo. We compare the measured anisotropy in the mock stellar halos with
that from their sphericalized versions where all the shape and substructure
induced anisotropies are erased. The growth of spatial anisotropy persists
throughout the entire halo when the bound satellites are present but remains
limited within the inner halo ($<60 \, h^{-1}\, {\rm kpc}$) after their
exclusion. This indicates that the spatial anisotropy in the inner halo is
induced by the diffuse substructures and the halo shape whereas the outer halo
anisotropy is dominated by the bound satellites. We find that the outer parts
of the stellar halo are kinematically colder than the inner regions. The
stellar orbits are predominantly radial but they become rotationally dominated
at certain radii that are marked by the prominent $\beta$ dips. Most of the
$\beta$ dips disappear after the removal of the satellites. A few shallow and
broad $\beta$ dips arise occasionally due to the presence of diffuse streams
and clouds. Our analysis suggests that a combined study of the spatial and
velocity anisotropies can reveal the structure and the assembly history of the
stellar halos.
