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We present 3D hydrodynamical simulations of ram‐pressure stripping of a disc galaxy orbiting in a galaxy cluster. In this paper, we focus on the properties of the galaxies' tails of stripped gas. The galactic wakes show a flaring width, where the flaring angle depends on the gas disc's cross‐section with respect to the galaxy's direction of motion. The velocity in the wakes shows a significant turbulent component of a few . The stripped gas is deposited in the cluster rather locally, i.e. within  from where it was stripped. We demonstrate that the most important quantity governing the tail density, length and gas mass distribution along the orbit is the galaxy's mass‐loss per orbital length. This in turn depends on the ram pressure as well as the galaxy's orbital velocity.  For a sensitivity limit of  in projected gas density, we find typical tail lengths of . Such long tails are seen even at large distances (0.5 to ) from the cluster centre. At this sensitivity limit, the tails show little flaring, but a width similar to the gas disc's size.  Morphologically, we find good agreement with the H  i  tails observed in the Virgo cluster by Chung et al. 2007. However, the observed tails show a much smaller velocity width than predicted from the simulation. The few known X‐ray and Hα tails are generally much narrower and much straighter than the tails in our simulations. Thus, additional physics like a viscous intracluster medium (ICM), the influence of cooling and tidal effects may be needed to explain the details of the observations.  We discuss the hydrodynamical drag as a heat source for the ICM but conclude that it is not likely to play an important role, especially not in stopping cooling flows.

Ram‐pressure stripping of disc galaxies orbiting in clusters – II. Galactic wakes