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A fraction of dwarf galaxies in the Virgo cluster contain disk features likebars and spiral arms. Using $N$-body simulations, we investigate the effects oftidal forces on the formation of such disk features in disk dwarf galaxiesresembling VCC856. We consider 8 Cluster-Galaxy models in which disk dwarfgalaxies with differing pericenter distance and spin orientation experience thetidal gravitational force of a Virgo-like NFW halo, and additional 8Galaxy-Galaxy models in which two dwarf galaxies undergo tidal interactionswith different strength. We find that the cluster tidal effect is moderate dueto the small galaxy size, making the bars form earlier by $\sim1$--$1.5\Gyr$compared to the cases in isolation. While the galactic halos significantly losetheir mass within the virial radius due to the cluster tidal force, the mass ofthe stellar disks is nearly unchanged, suggesting that the inner regions of adisk-halo system is secured from the tidal force. The tidal forcing from eitherthe cluster potential or a companion galaxy triggers the formation of two-armedspirals at early time before a bar develops. The tidally-driven arms decay andwind with time, suggesting that they are kinematic density waves. In terms ofthe strength and pitch angle, the faint arms in VCC856 are best matched withthe arms in a marginally unstable galaxy produced by a distant tidal encounterwith its neighbor $\sim0.85\Gyr$ ago.

Origin of Non-axisymmetric Features of Virgo Cluster Early-type Dwarf Galaxies. II. Tidal Effects on Disk Features and Stability