  In this paper we compute the gravitational signal emitted when a white dwarf
moves around a black hole on a closed or open orbit using the affine model
approach. We compare the orbital and the tidal contributions to the signal,
assuming that the star moves in a safe region where, although very close to the
black hole, the strength of the tidal interaction is insufficient to provoque
the stellar disruption. We show that for all considered orbits the tidal signal
presents sharp peaks corresponding to the excitation of the star non radial
oscillation modes, the amplitude of which depends on how deep the star
penetrates the black hole tidal radius and on the type of orbit. Further
structure is added to the emitted signal by the coupling between the orbital
and the tidal motion.
