We describe the results of high resolution numerical simulations of string
seeded structure formation using a cosmic string network with either cold or
hot dark matter. The resulting linear power spectrum, ${\cal P}(k)$, of
density
perturbations is calculated and compared with the linear power spectrum
inferred from various galaxy surveys. We investigate
the performance of cosmic string models in open universes and flat
universes with a
non-zero cosmological constant and show that for $\Gamma \sim 0.1-0.2$ the
power spectrum
of cosmic string induced CDM fluctuations resembles the power spectrum
inferred
from various galaxy red-shift surveys. We find that $\sigma_8/G\mu_6 \sim
0.1-0.6$
for $0.5 \, \la \, h \, \la \, 0.7$ and
$0.1 \, \la \, \Omega_{CDM} \, \la \, 1$. The HDM scenario with cosmic
strings seems
to require a large scale dependent biasing in order to be consistent with
observations.
These results are qualitatively very similar to those obtained by Avelino,
Caldwell and Martins
using the semi-analytic formalism developed by Albrecht and Stebbins.