Abstract
We investigate pattern speeds in spiral galaxies where the structure is induced by an interaction with a companion galaxy. We perform calculations modeling the response of the stellar and/or gaseous components of a disc. Generally we do not find a unique pattern speed in these simulations, rather the pattern speed decreases with radius, and the pattern speed for individual spiral arms differ. The maximum pattern speed is ~20 km/s/kpc for the discs with a live stellar component, decreasing to 5 km/s/kpc at the edge of the spiral perturbation. When only the gas is modeled, Omega_p is typically very low (5 km/s/kpc) at all radii.
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