  We present detailed numerical simulations of NGC 1433, an intermediate-type
barred spiral showing strong morphological features including a secondary bar,
nuclear ring, inner ring, outer pseudoring, and two striking, detached spiral
arcs known as ``plumes.'' This galaxy is an ideal candidate for recreating the
observed morphology through dynamical models and determining the pattern speed.
We derived a gravitational potential from an $H$-band image of the galaxy and
simulated the behavior of a two-dimensional disk of 100,000 inelastically
colliding gas particles. We find that the closest matching morphology between a
$B$-band image and a simulation occurs with a pattern speed of 0.89 km s$^{-1}$
arcsec$^{-1}$ $\pm$ 5-10%. We also determine that the ratio of corotation
radius to the average published bar radius is 1.7 $\pm$ 0.3, with the ambiguity
in the bar radius being the largest contributor to the error.
