Binary neutron star mergers and short gamma-ray bursts: Effects of magnetic field orientation, equation of state, and mass ratio

Abstract

We present fully GRMHD simulations of the merger of binary neutron star (BNS) systems. We consider BNSs producing a hypermassive neutron star (HMNS) that collapses to a spinning black hole (BH) surrounded by a magnetized accretion disk in a few tens of ms. We investigate whether such systems may launch relativistic jets and power short gamma-ray bursts. We study the effects of different equations of state (EOSs), different mass ratios, and different magnetic field orientations. For all cases, we present a detailed investigation of the matter dynamics and of the magnetic field evolution, with particular attention to its global structure and possible emission of relativistic jets. The main result of this work is that we found the formation of an organized magnetic field structure. This happens independently of EOS, mass ratio, and initial magnetic field orientation. We also show that those models that produce a longer-lived HMNS lead to a stronger magnetic field before collapse to BH. Such larger fields make it possible, for at least one of our models, to resolve the MRI and hence further amplify the magnetic field. However, by the end of our simulations, we do not observe a magnetically dominated funnel and hence neither a relativistic outflow. With respect to the recent simulations of Ruiz et al 2016, we evolve models with lower and more realistic initial magnetic field strengths and, because of computational reasons, we do not evolve the accretion disk for the long timescales that seem to be required in order to see a relativistic outflow. Since all our models produce a similar ordered magnetic field structure, we expect that the results found in Ruiz et al 2016, where they only considered an equal-mass system with an ideal fluid EOS, should be general and, at least from a qualitative point of view, independent from mass-ratio, magnetic field orientation, and EOS.