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• W2616831680 abstract "The merger of binary neutron stars, or of a neutron star and a stellar-mass black hole, can result in the formation of a massive rotating torus around a spinning black hole. In addition to providing collimating media for gamma-ray burst jets, unbound outflows from these disks are an important source of mass ejection and rapid neutron capture (r-process) nucleosynthesis. We present the first three-dimensional general-relativistic magnetohydrodynamic (GRMHD) simulations of neutrino-cooled accretion disks in neutron star mergers, including a realistic equation of state valid at low densities and temperatures, self-consistent evolution of the electron fraction, and neutrino cooling through an approximate leakage scheme. After initial magnetic field amplification by magnetic winding, we witness the vigorous onset of turbulence driven by the magneto-rotational instability (MRI). The disk quickly reaches a balance between heating from MRI-driven turbulence and neutrino cooling, which regulates the midplane electron fraction to a low equilibrium value $Y_text{e} approx 0.1$. Over the 380 ms duration of the simulation, we find that a fraction $approx 20%$ of the initial torus mass is unbound in powerful outflows with velocities $v approx 0.03-0.1,c$ and electron fractions $Y_text{e} approx 0.1-0.25$. Post-processing the outflows through a nuclear reaction network shows the production of a robust second and third peak r-process. Though broadly consistent with the results of previous axisymmetric hydrodynamical simulations, extrapolation of our results to late times suggests that the total ejecta mass from GRMHD disks is significantly higher. Our results provide strong evidence that post-merger disk outflows are an important site for the r-process." @default.
• W2616831680 created "2017-05-26" @default.
• W2616831680 creator A5011305019 @default.
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• W2616831680 date "2017-12-06" @default.
• W2616831680 modified "2023-10-14" @default.
• W2616831680 title "Three-Dimensional General-Relativistic Magnetohydrodynamic Simulations of Remnant Accretion Disks from Neutron Star Mergers: Outflows and <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline><mml:mi>r</mml:mi></mml:math> -Process Nucleosynthesis" @default.
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• W2616831680 doi "https://doi.org/10.1103/physrevlett.119.231102" @default.
• W2616831680 hasPubMedId "https://pubmed.ncbi.nlm.nih.gov/29286684" @default.
• W2616831680 hasPublicationYear "2017" @default.
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