  We examine the observable properties of simulated barred galaxies including
radial mass profiles, edge-on structure and kinematics, bar lengths and pattern
speed evolution for detailed comparison to real systems. We have run several
simulations in which bars are created through inherent instabilities in
self-consistent simulations of a realistic disc+halo galaxy model with a
disc-dominated, flat rotation curve. These simulations were run at high (N=20M
particles) and low (N=500K) resolution to test numerical convergence. We
determine the pattern speeds in simulations directly from the phase angle of
the bar versus time and the Tremaine-Weinberg method. Fundamental dynamics do
not change between the high and low resolution, suggesting that convergence has
been reached in this case. We find the higher resolution is needed to simulate
structural and kinematic properties accurately. The edge-on view of the
higher-resolution system clearly shows the bending instability and formation of
a peanut-shaped bulge. We determined bar lengths by different means to
determine the simulated bar is fast, with a corotation to bar length ratio
under 1.5. Simulated bars in these models form with pattern speeds slower than
those observed and slow down during their evolution. Dynamical friction between
the bar and dark halo is responsible for this deceleration, as revealed by the
transfer of angular momentum between the disc and the halo. However, even
though the pattern speed is reduced at later times, the instantaneous scale
length of the disc has grown sufficiently for the bar motion to agree with many
observations. By using a different model and simulation technique than other
authors, we are able to compare the robustness of these methods.
