the merger of magnetized neutron stars can provide the basic conditions for the central engine of SGRBs.

Considerable effort has also been dedicated to investigating the properties of the HMNS under more controlled conditions. For instance, using ultrahigh spatial resolutions but axisymmetric initial data, Ref.  [@Siegel2013] has provided the first evidence from three-dimensional global simulations that a magnetorotational instability (MRI) [@Velikhov1959; @Chandrasekhar1960] is likely to develop during the lifetime of the HMNS (see also Refs. [@Duez:2006qe; @Duez2006a] for earlier work in two dimensions). In addition, again using axisymmetric initial data and different magnetic field configurations, it has been shown that a magnetically driven wind can be launched from the outer layers of the HMNS as a result of its differential rotation [@Kiuchi2012b; @Siegel2014]. These works have also highlighted that for realistic magnetic field topologies the wind is baryon loaded and quasi-isotropic, with bulk velocities of $\sim 0.1\,c$ [@Siegel2014]. More recently, instead, the use of subgrid modeling as an effective way to describe the turbulent dynamics that develops in the shear layer between the two neutron stars at merger, has suggested that amplifications of up to 5 orders of magnitude are possible [@Giacomazzo:2014b], although these amplifications are not produced in direct 