Abstract
A combined particle-mesh N-body/gridded hydrodynamics/stellar evolution code is employed to model the response of a galaxy disk to an impulsive perturbation. The resulting galaxy is examined for asymmetry in morphology and dynamics to answer the question of whether free librations in the plane of the disk can explain the relatively large proportion of asymmetric field spirals. The simulation produced a perturbed disk containing streamers of gas and stars, gas shocks, and m = 1 and m = 2 spiral structure. Strong kinematic peculiarities were generated as well. However, although the resulting disk reproduced many of the kinematic features observed in H I synthesis maps, the effects are relatively short-lived, lasting only on the order of a dynamical timescale. The similarities between the model and the tidally deformed galaxy NGC 5474, however, do leave open the possibility of forced sloshing modes playing a role in galaxies undergoing tidal interactions.
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