  We study theoretically how the initial cosmological conditions establish the
dependence of galaxy properties on the environment. First, we adopt the linear
tidal torque theory according to which the angular momentum of a proto-galaxy
is generated at first order by the misalignment between the proto-galaxy
inertia tensor and the local tidal tensor. Then, we quantify analytically the
degree of the misalignment between the two tensors, and show quantitatively
that it increases as the density of the environment decreases. It implies that
the proto-galaxies forming in the lower density regions should end up with
having higher angular momentum than those in the higher density regions, which
is consistent with recent numerical finding that the void and field galaxies
have higher spin parameters than the cluster galaxies. Since the galaxy angular
momentum plays a role of developing a disk-like structure and hindering the
star-formation, our theoretical insight provides an answer to such fundamental
observational question as why the large void galaxies have young stellar
populations and high specific star formation rate, which was not explained by
the previous morphology-density relation.
