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The detection of binary neutron star mergers represents one of the mostimportant and complex astrophysical discoveries of the recent years. One of theunclear aspects of the problem is the turbulent magnetic field amplification,initially triggered by the Kelvin-Helmholtz instability at much smaller scalesthan any reachable numerical resolution nowadays. Here we present numericalsimulations of the first ten milliseconds of a binary neutron star merger.First, we confirm in detail how the simulated amplification depends on thenumerical resolution and is distributed on a broad range of scales, as expectedfrom turbulent MHD theory. We find that an initial large-scale magnetic fieldof $10^{11}\,$G inside each star is amplified in the remnant toroot-mean-square values above $10^{16}\,$G within the first $5$ millisecondsfor our highest-resolution run. Then, we run large eddy simulations, exploringthe performance of the subgrid-scale gradient model, already testedsuccessfully in previous turbulent box simulations. We show that the additionof this model is especially important in the induction equation, since it leadsto an amplification of the magnetic field comparable to a higher-resolutionrun, but with a greatly reduced computational cost. In the first 10milliseconds, there is no clear hint for an ordered, large-scale magneticfield, which should indeed occur in longer timescales through magnetic windingand the magneto-rotational instability.

physical review. d/physical review. d.

Turbulent magnetic-field amplification in the first 10 milliseconds  after a binary neutron star merger: comparing high-resolution and large eddy  simulations