GW170817 and GRB 170817A provided direct evidence that binary neutron star (NSNS) mergers can produce short gamma-ray bursts (sGRBs). However, questions remain about the nature of the central engine. Depending on the mass, the remnant from a NSNS merger may promptly collapse to a black hole (BH), form a hypermassive neutron star (HMNS) which undergoes a delayed collapse to a BH, a supramassive neutron star (SMNS) with a much longer lifetime, or an indefinitely stable normal NS. There is strong evidence that a BH with an accretion disk can launch a sGRB-compatible jet via the Blandford–Znajek mechanism, but whether a supramassive star can do the same is less clear. We have performed general relativistic magnetohydrodynamics (GRMHD) simulations of the merger of both irrotational and spinning, equal-mass NSNSs constructed from a piecewise polytropic representation of the nuclear SLy equation of state, with a range of gravitational (ADM) masses that yield remnants with mass above and below the mass-shedding (Kepler) limit. Each NS is endowed with a dipolar magnetic field extending from the interior into the exterior, as in a radio pulsar. We examine cases with different initial binary masses, both a case which produces a HMNS which collapses to a BH, and lower mass binaries that produce SMNS remnants. We find similar jet-like structures (helical magnetic field structures, a magnetically dominated evacuated funnel and mildly relativistic outflow from the poles) for both the SMNS and HMNS remnants that meet our basic critera for an incipient jet. The outflow for the HMNS case is consistent with a Blandford-Znajek (BZ) jet. There is sufficient evidence that such BZ-powered outflows can break out and produce ulrarelativistic jets that we can describe the HMNS system as a sGRB progenitor. However, the incipient jets from the SMNS remnants have much more baryon pollution and we see indications of inefficient acceleration and mixing with the surrounding debris torus. Therefore, we conclude that outflows from SMNSs cannot be the progenitors of sGRBs.
Movies Nawaf Aldrees, Jamie Bamber, Jonah Doppelt, Yinuan Liang, Rohan Narasimhan, Milton Ruiz, Stuart L. Shapiro, Antonios Tsokaros, and Eric Yu
Irrotational binary with ADM mass $M=2.40 M_\odot$. Supramassive remnant.
Irrotational binary with ADM mass $M=2.40 M_\odot$. Supramassive remnant. h× Polarization (Lower Hemisphere)
Irrotational binary with ADM mass $M=2.40 M_\odot$. Supramassive remnant. h+ Polarization (Surface Plot of Equatorial Plane)
Irrotational binary with ADM mass $M=2.54 M_\odot$. Supramassive remnant.
Irrotational binary with ADM mass $M=2.54 M_\odot$. Supramassive remnant. h× Polarization (Lower Hemisphere)
Irrotational binary with ADM mass $M=2.54 M_\odot$. Supramassive remnant. h+ Polarization (Surface Plot of Equatorial Plane)
Irrotational binary with ADM mass $M=2.57 M_\odot$. Supramassive remnant.
Irrotational binary with ADM mass $M=2.57 M_\odot$. Supramassive remnant. h× Polarization (Lower Hemisphere)
Irrotational binary with ADM mass $M=2.57 M_\odot$. Supramassive remnant. h+ Polarization (Surface Plot of Equatorial Plane)
Irrotational binary with ADM mass $M=2.57 M_\odot$. Supramassive remnant. 2D Movie
Irrotational binary with ADM mass $M=2.70 M_\odot$. Hypermassive remnant that collapses to a black hole.
Irrotational binary with ADM mass $M=2.70 M_\odot$. Hypermassive remnant that collapses to a black hole. h× Polarization (Lower Hemisphere)
Irrotational binary with ADM mass $M=2.70 M_\odot$. Hypermassive remnant that collapses to a black hole. h+ Polarization (Surface Plot of Equatorial Plane)
Irrotational binary with ADM mass $M=2.70 M_\odot$. Hypermassive remnant that collapses to a black hole. 2D Movie
Spinning binary with $\chi_{NS}=0.27$ and ADM mass $M=2.51 M_\odot$. Supramassive remnant.
Spinning binary with $\chi_{NS}=0.27$ and ADM mass $M=2.51 M_\odot$. Supramassive remnant. h× Polarization (Lower Hemisphere)
Spinning binary with $\chi_{NS}=0.27$ and ADM mass $M=2.51 M_\odot$. Supramassive remnant. h+ Polarization (Surface Plot of Equatorial Plane)
Spinning binary with $\chi_{NS}=0.26$ and ADM mass $M=2.57 M_\odot$. Supramassive remnant.
Spinning binary with $\chi_{NS}=0.26$ and ADM mass $M=2.57 M_\odot$. Supramassive remnant. h× Polarization (Lower Hemisphere)
Spinning binary with $\chi_{NS}=0.26$ and ADM mass $M=2.57 M_\odot$. Supramassive remnant. h+ Polarization (Surface Plot of Equatorial Plane)