  I present results from numerical N-body simulations regarding the effect of
merging events on the angular momentum distribution of galactic halos as well
as a comparison of halo growth in Press-Schechter vs. N-body methods. A total
of six simulations are used spanning 3 cosmologies: a standard flat Omega_0=1
model, an open Omega_0=0.3 model and a "tilted" flat Omega_0=1 model with
spectral index n=0.8. In each model, one run was conducted using a spatially
uniform grid of particles and one using a refined grid in a large void. In all
three models and all environments tested, the mean angular momentum of merger
remnants (halo interaction products with mass ratios 3:1 or less) is greater
than non-merger remnants. Furthermore, the dispersion in the merger-remnant
angular momentum distribution is smaller than the dispersion of the non-merger
distribution. The interpretation most consistent with the data is that the
orbital angular momentum of the interactors is important in establishing the
final angular momentum of the merger product. I give the angular momentum
distribution which describes the merger remnant population.
  I trace the most massive progenitor of L_* galactic-mass halos (uniform grid)
and 10^{11} solar mass halos (refined void) from redshift z=0 back to z=5.
Monte-Carlo mass histories match simulations reasonably well for the latter
sample. I find that for halos of mass 10^{12} to 10^{14} solar masses, this
method can underestimate the mass of progenitors by 20%, hence yielding
improper formation redshifts of halos. With this caveat, however, the general
shapes of halo mass histories and formation-time distributions are preserved.
