yields the Maxwell equations in vacuum, thus allowing for the study of the magnetic-field evolution also well outside the stellar magnetosphere [@Palenzuela:2008sf].

Partly because of the increased complexity of the equations and partly because of the additional difficulties posed by their numerical solution (the equations easily become stiff in regions of high conductivity), RMHD simulations have started only rather recently. Most of the work so far has focussed on problems in flat spacetimes [@Dumbser2009; @Komissarov2007; @Palenzuela:2008sf; @Zenitani2010; @Zanotti2011b; @Takamoto2011b; @Mizuno2013], but general-relativistic investigations have also been carried out on fixed spacetimes [@Bucciantini2012a]. Indeed, together with the work carried out in Refs. [@Palenzuela2013a; @Ponce2014], those reported here are, to the best of our knowledge, the only RMHD simulations of the dynamics of binary neutron stars in general relativity. More specifically, we have followed the inspiral, merger, and collapse to a black hole of a neutron-star binary in which the stars have the same gravitational mass of $M=1.625\,{M_{\odot}}$ and are modelled with a simple ideal-fluid EOS.

Complementing the work reported in Refs. [@Palenzuela2013a; @Ponce2014], which concentrated on the electromagnetic emission during the inspiral and at the merger, the focus of the simulations reported here is that of assessing the impact that resistive 