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We present a phenomenological description of the properties of tidal tailsforming around dwarf galaxies orbiting the Milky Way. For this purpose we usecollisionless N-body simulations of dwarfs initially composed of a diskembedded in an NFW dark matter halo. The dwarfs are placed on seven orbitsaround the Milky Way-like host, differing in size and eccentricity, and theirevolution is followed for 10 Gyr. In addition to the well-studied morphologicaland dynamical transformation of the dwarf's main body, the tidal strippingcauses them to lose a substantial fraction of mass both in dark matter andstars which form pronounced tidal tails. We focus on the properties of thestellar component of the tidal tails thus formed. We first discuss the breakradii in the stellar density profile defining the transition to tidal tails asthe radii where the profile becomes shallower and relate them to theclassically defined tidal radii. We then calculate the relative density andvelocity of the tails at a few break radii as a function of the orbital phase.Next, we measure the orientation of the tails with respect to an observerplaced at the centre of the Milky Way. The tails are perpendicular to this lineof sight only for a short period of time near the pericentre. For most of thetime the angles between the tails and this line of sight are low, withorbit-averaged medians below 42 degrees for all, even the almost circularorbit. The median angle is typically lower while the maximum relative densityhigher for more eccentric orbits. The combined effects of relative density andorientation of the tails suggest that they should be easiest to detect fordwarf galaxies soon after their pericentre passage.

Tidal tails of dwarf galaxies on different orbits around the Milky Way