Magnetohydrodynamic Simulations of Binary Neutron Star Mergers in General Relativity: Effects of Magnetic Field Orientation on Jet Launching

Milton Ruiz; Antonios Tsokaros; Stuart L. Shapiro

doi:10.1103/PhysRevD.101.064042

paper

Magnetohydrodynamic Simulations of Binary Neutron Star Mergers in General Relativity: Effects of Magnetic Field Orientation on Jet Launching

arXiv:2001.09153 · doi:10.1103/PhysRevD.101.064042

Abstract

Binary neutron star (NSNS) mergers can be sources of gravitational waves coincident with electromagnetic counterpart emission. To solidify their role as multimessenger sources, we present fully 3D, general relativistic, magnetohydrodynamic simulations of spinning NSNSs initially on quasicircular orbits that merge and undergo delayed collapse to a black hole (BH). The NSNSs consist of two identical stars modeled as $Γ = 2$ polytropes with spin $χ_{N S} = 0.36$ aligned along the direction of the total orbital angular momentum $L$ . Each star is initially threaded by a dynamical unimportant interior dipole B-field. The field is extended into the exterior where a nearly force-free magnetosphere resembles that of a pulsar. The magnetic dipole moment $μ$ is either aligned or perpendicular to $L$ and has the same initial magnitude for each orientation. For comparison, we also impose symmetry across the orbital plane in one case where $μ$ in both stars is aligned along $L$ . We find that the lifetime of the transient hypermassive neutron star remnant, the jet launching time, and the ejecta are very sensitive to the B-field orientation. By contrast, the physical properties of the BH + disk remnant, such as the mass and spin of the BH, the accretion rate, and the electromagnetic luminosity, are roughly independent of the initial B-field orientation. In addition, we find imposing symmetry across the orbital plane does not play a significant role in the final outcome of the mergers. Our results show that an incipient jet emerges only when the seed B-field has a sufficiently large-scale poloidal component aligned to $L$ . The lifetime [ $Δ t ≳ 140 (M_{N S} /1.625 M_{⊙}) ms$ ] and Poynting luminosities [ $L_{E M} ≃ 1 0^{52}$ erg/s] of the jet, when it forms, are consistent with typical short gamma-ray bursts, as well as with the Blandford--Znajek mechanism for launching jets.

arXiv comment16 pages, 12 figures. Matches published version

Magnetohydrodynamic Simulations of Binary Neutron Star Mergers in General Relativity: Effects of Magnetic Field Orientation on Jet Launching

Abstract

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