the tidal tails of both clusters. The background is the grey-scale density map of Gaia DR2 (©ESA/Gaia/DPAC). This composite image has been produced using the facilities of Aladin Desktop[^3].

![The tidal tails of Praesepe (yellow) and the Hyades (cyan) over-plotted to the Gaia DR2 sky using TOPCAT and Aladin facilities. []{data-label="Figure5"}](Figure5.jpg){width="49.00000%"}

A comparison with a theoretical model from N-body calculations for an 650 Myr old cluster (Hyades) showed very good coincidence with regard to the location of the tidal tails of Praesepe, too. After the findings in Paper I, this is another very satisfactory confirmation for both theory and observations, in general. In detail, we observe for both clusters that the preceding tail is more pronounced than the trailing one, though we have good reasons to suspect that this is due to different causes. In the case of Praesepe the trailing tail stretches to larger distances from the Sun and probably suffers from the incompleteness of our sample at fainter stars. Both Hyades tails are located at about the same distance from the Sun but the trailing tail of the Hyades shows an inhomogeneous structure and may have been shredded by shocks or collisions in the past. Moreover, the proportion 