here we are mostly interested in assessing the differences introduced in the dynamics of the BMP by resistive effects. These effects suffer from even larger uncertainties than those associated to the different EOSs.

Adaptive mesh refinement and symmetries
---------------------------------------

Our code makes use of the `Cactus` [@cactus_url] computational framework, which allows us to employ a box-in-box vertex-centered adaptive mesh refinement grid hierarchy that tracks the “center of mass” of the stars as they orbit each other. This was achieved via the `BNSTracker` thorn implemented by W. Kastaun and the `Carpet` driver [@Schnetter-etal-03b]. The numerical domain consists of six levels of refinement with the resolution doubling between adjacent refinements. In addition, we employ moving refinement boxes in order to track the high-density regions. The outer boundary of the computational domain is located at $\approx 378\,{{\rm km}}$. The finest resolution during the inspiral and merger is $\Delta x\approx 296~{{\rm m}}$, but an extra refinement level is activated right after the merger with a resolution of $\Delta x\approx 148~{{\rm m}}$. It is important to remark that, although in a small region of spatial extent $\sim 13.5\,{{\rm km}}$, this resolution is considerably higher than the one used in Ref. [@Rezzolla:2011] ([i.e., ]{}$\approx 221\,{{\rm m}}$ 