effects have on the dynamics of the binary after the merger and through to collapse to a black hole. To this scope we have carried out a close comparison with an equivalent simulation performed for the same binary within the traditional IMHD approximation. In this way it has been possible to determine both the similarities between the two regimes and the novel features. The most important of such features is the evidence the survival time of the HMNS before collapse to a black hole increases in a RMHD simulation. This difference is associated to a less efficient magnetic braking in the resistive regime, in which matter is no longer perfectly advected with the flow, but can move across magnetic-field lines. In turn, this reduces the transport of angular momentum away from the central regions of the HMNS, increasing its lifetime. Interestingly, a longer-lived magnetized HMNS is of help in those models of SGRBs which invoke the existence of a magnetarlike object produced after the merger [@Zhang2001; @Metzger2008; @Metzger:2011; @Bucciantini2012; @Rezzolla2014b; @Ciolfi2014]. Another important result of the simulations reported here, which have been performed at higher resolutions and with a different grid structure than those in the previous work of Ref. 