  Bars in galaxies may develop through a global instability or due to an
interaction with another system. We study bar formation in disky dwarf galaxies
orbiting a Milky Way-like galaxy. We employ $N$-body simulations to study the
impact of initial orbital parameters: the size of the dwarf galaxy orbit and
the inclination of its disc with respect to the orbital plane. In all cases a
bar develops in the center of the dwarf during the first pericenter on its
orbit around the host. Between subsequent pericenter passages the bars are
stable, but at the pericenters they are usually weakened and shortened. The
initial properties and details of the further evolution of the bars depend
heavily on the orbital configuration. We find that for the exactly prograde
orientation, the strongest bar is formed for the intermediate-size orbit. On
the tighter orbit, the disc is too disturbed and stripped to form a strong bar.
On the wider orbit, the tidal interaction is too weak. The dependence on the
disc inclination is such that weaker bars form in more inclined discs. The bars
experience either a very weak buckling or none at all. We do not observe any
secular evolution, possibly because the dwarfs are perturbed at each pericenter
passage. The rotation speed of the bars can be classified as slow
($R_\mathrm{CR}/l_\mathrm{bar}\sim2-3$). We attribute this to the loss of a
significant fraction of the disc's rotation during the encounter with the host
galaxy.
