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Major mergers between massive clusters have a profound effect in theintracluster gas, which may be used as a probe of the dynamics of structureformation at the high end of the mass function. An example of such a merger isobserved at the northern component of Abell 1758, comprised of two massivesub-clusters separated by approximately 750 kpc. One of the clusters exhibitsan offset between the dark matter and the intracluster gas. We aim to determinewhether it is possible to reproduce the specific morphological features of thiscluster by means of a major merger. We perform dedicated SPH (smoothed particlehydrodynamics) N-body simulations in an attempt to simultaneously recoverseveral observed features of Abell 1758, such as the X-ray morphology and theseparation between the two peaks in the projected galaxy luminosity map. Wepropose a specific scenario for the off-axis collision of two massive clusters.This model adequately reproduces several observed features and suggests thatAbell 1758 is seen approximately 0.4 Gyr after the first pericentric passage,and that the clusters are already approaching their maximum separation. Thismeans that their relative velocity is as low as 380 km/s. At the same time, thesimulated model entails shock waves of ~4500 km/s, which are currentlyundetected presumably due to the low-density medium. We explain the differencebetween these velocities and argue that the predicted shock fronts, whileplausible, cannot be detected from currently available data.

Simulating the shocks in the dissociative galaxy cluster Abell 1758N