In the most extreme case, this constitutes a short-term (<50 Myr) SFR increase of 50 % over the non-merging galaxies experiencing ram pressure. There, our simulations show SFRs of up to 20 M ⊙ yr -1 (compared to 3 M ⊙ yr -1 of the non-merging galaxies in vacuum). The SFRs peak at the time of the galaxies first fly-through. Results: Averaged over the simulation time (1 Gyr) the merging pairs show a negligible 5% enhancement in SFR, when compared to single galaxies under the same environmental conditions. Each simulation in the ICM is compared to simulations of the merger in vacuum and the non-merging galaxies with acting ram pressure. Ram pressure is kept constant within a simulation time period, as is the ICM temperature of 10 7 K. Furthermore, we vary the properties of the intracluster medium (ICM) in rough steps: the speed of the merging system relative to the ICM between 5 km s -1, the ICM density between 10 -29 and 10 -27 g cm -3, and the ICM direction relative to the mergers' orbital plane. We sample different geometric configurations of the merging systems (edge-on and face-on mergers, different impact parameters). In our simulations, we vary mass ratios between 1:4 and 1:8 in a binary merger. The code features a threshold-based statistical recipe for star formation, as well as radiative cooling and modeling of galactic winds. Methods: We make use of the combined N-body/hydrodynamic code GADGET-2. Our goal is to provide an estimate of the combined effect of merging and RPS compared to the influence of the individual processes. We are concerned with the changes in stripping efficiency and the time evolution of the star formation rate. Aims: We investigate the effect of ram pressure stripping (RPS) on several simulations of merging pairs of gas-rich spiral galaxies.
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