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Using self-consistent three-dimensional (3D) N-body simulations, weinvestigate the physical properties of non-axisymmetric features in a diskgalaxy created by a tidal interaction with its companion. The primary galaxyconsists of a stellar disk, a bugle, and a live halo, corresponding toMilky-Way type galaxies, while the companion is represented by a halo alone. Wevary the companion mass and the pericenter distance to explore situations withdiffering tidal strength parameterized by either the relative tidal force P orthe relative imparted momentum S. We find that the formation of a tidal tail inthe outer parts requires P > 0.05 or S > 0.07. A stronger interaction resultsin a stronger, less wound tail that forms earlier. Similarly, a stronger tidalforcing produces stronger, more loosely wound spiral arms in the inner parts.The arms are approximately logarithmic in shape, with both amplitude and pitchangle decaying with time. The derived pattern speed decreases with radius andis close to the Omega-kappa/2 curve at late time, with Omega and kappa denotingthe angular and epicycle frequencies, respectively. This suggests that thetidally-induced spiral arms are most likely kinematic density waves weaklymodified by self-gravity. Compared to the razor-thin counterparts, arms in the3D models are weaker, have a smaller pitch angle, and wind and decay morerapidly. The 3D density structure of the arms is well described by theconcentrated and sinusoidal models when the arms are in the nonlinear andlinear regimes, respectively. We demonstrate that dynamical friction betweeninteracting galaxies transfers the orbital angular momentum of one galaxy tothe spin angular momentum of the companion halo.

Physical Properties of Tidal Features of Interacting Disk Galaxies: Three-dimensional Self-consistent Models