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The merger of binary neutron stars (BNSs) can lead to large amplifications ofthe magnetic field due to the development of turbulence and instabilities inthe fluid, such as the Kelvin-Helmholtz shear instability, which drivesmall-scale dynamo activity. In order to properly resolve such instabilitiesand obtain the correct magnetic field amplification, one would need to employresolutions that are currently unfeasible in global general relativisticmagnetohydrodynamic (GRMHD) simulations of BNS mergers. Here, we present asubgrid model that allows global simulations to take into account thesmall-scale amplification of the magnetic field which is caused by thedevelopment of turbulence during BNS mergers. Assuming dynamo saturation, weshow that magnetar-level fields ($\sim 10^{16}\,{\rm G}$) can be easilyreached, and should therefore be expected from the merger of magnetized BNSs.The total magnetic energy can reach values up to $\sim 10^{51}\,{\rm erg}$ andthe post-merger remnant can therefore emit strong electromagnetic signals andpossibly produce short gamma-ray bursts.

Producing Magnetar Magnetic Fields in the Merger of Binary Neutron Stars