  We use N-body simulations to investigate the evolution of the orientation and
magnitude of dark matter halo angular momentum within the large scale structure
since z=3. We look at the evolution of the alignment of halo spins with
filaments and with each other, as well as the spin parameter, which is a
measure of the magnitude of angular momentum. It was found that the angular
momentum vectors of dark matter haloes at high redshift have a weak tendency to
be orthogonal to filaments and high mass haloes have a stronger orthogonal
alignment than low mass haloes. Since z=1, the spins of low mass haloes have
become weakly aligned parallel to filaments, whereas high mass haloes kept
their orthogonal alignment. This recent parallel alignment of low mass haloes
casts doubt on tidal torque theory as the sole mechanism for the build up of
angular momentum. We see evidence for bulk flows and the broadening of
filaments over time in the alignments of halo spin and velocities. We find a
significant alignment of the spin of neighboring dark matter haloes only at
very small separations, $r<0.3$Mpc/h, which is driven by substructure. A
correlation of the spin parameter with halo mass is confirmed at high redshift.
