  High resolution gravity plus smoothed particle hydrodynamics simulations are
used to study the formation of galaxies within the context of hierarchical
structure formation. The simulations have sufficient dynamic range to resolve
from ten kpc scale galactic disks up to many Mpc scale filaments. Over this
range of scales, we find that hierarchical structure development proceeds
through a series of increasingly larger filamentary collapses. The well
resolved simulated galaxies contain hundreds to thousands of particles and have
varied morphologies covering the entire expected range from disks to tidally
distorted objects. The epoch of galaxy formation occurs early, about redshift
2.5 for 10^12 M_sun galaxies. Hierarchical formation naturally produces
correlations among the mass, age, morphology, and local density of galaxies
which match the trends in the observed morphology--density relation. We also
describe a method of spiral galaxy formation in which galactic disks form
through the discrete accretion of gas clouds which transport most of the
angular momentum to the inner regions. Such a process is characteristic of the
somewhat chaotic nature of hierarchical structure formation where simple
analytical ideas of spherical collapse appear incongruous.
