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Mergers of gas-rich galaxies are key events in the hierarchical built-up ofcosmic structures, and can lead to the formation of massive black holebinaries. By means of high-resolution hydrodynamical simulations we considerthe late stages of a gas-rich major merger, detailing the dynamics of twocircumnuclear discs, and of the hosted massive black holes during their pairingphase. During the merger gas clumps with masses of a fraction of the black holemass form because of fragmentation. Such high-density gas is very effective informing stars, and the most massive clumps can substantially perturb the blackhole orbits. After $\sim 10$ Myr from the start of the merger a gravitationallybound black hole binary forms at a separation of a few parsecs, and soon after,the separation falls below our resolution limit of $0.39$ pc. At the time ofbinary formation the original discs are almost completely disrupted because ofSNa feedback, while on pc scales the residual gas settles in a circumbinarydisc with mass $\sim 10^5 M_\odot$. We also test that binary dynamics is robustagainst the details of the SNa feedback employed in the simulations, while gasdynamics is not. We finally highlight the importance of the SNa time-scale onour results.

Massive black hole and gas dynamics in mergers of galaxy nuclei - II. Black hole sinking in star-forming nuclear discs