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Structure of Stable Binary Neutron Star Merger Remnants: Role of Initial Spin
High Energy Astrophysical Phenomena · Submitted 12 Dec 2016
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We present visualizations of the fluid flow and temperature distribution and find a strong impact of the spin on vortex structure and nonaxisymmetric deformation.
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The abstract, sentence by sentence
We present general relativistic numerical simulations of binary neutron star (BNS) mergers with different initial spin configurations. We focus on models with stars of mass 1.4 M_sol each, which employ the equation of state (EOS) by Shen, Horowitz, and Teige, and which result in stable NSs as merger remnants. For comparison, we consider two irrotational equal mass (M=1.35 M_sol) and unequal mass (M=1.29,1.42 M_sol) BNS models using the APR4 EOS, which result in a supramassive merger remnant. We present visualizations of the fluid flow and temperature distribution and find a strong impact of the spin on vortex structure and nonaxisymmetric deformation. We compute the radial mass distribution and the rotation profile in the equatorial plane using recently developed measures independent of spatial gauge, revealing slowly rotating cores that can be well approximated by the cores of spherical stars. We also study the influence of the spin on the inspiral phase and the gravitational wave (GW) signal. Using a newly developed analysis method, we further show that gravitational waveforms from BNS mergers can exhibit one or more phase jumps after merger, which occur together with minima of the strain amplitude. We provide a natural explanation in terms of the remnant's quadrupole moment, and show that cancellation effects due to phase jumps can have a strong impact on the GW power spectrum. Finally, we discuss the impact of the spin on the amount of ejected matter.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present general relativistic numerical simulations of binary neutron star (BNS) mergers with different initial spin configurations. | contribution 0.85 | 0.96 | 0.03 | asserted 0.95 |
| s1 | We focus on models with stars of mass 1.4 M_sol each, which employ the equation of state (EOS) by Shen, Horowitz, and Teige, and which result in stable NSs as merger remnants. | method 0.95 | 0.84 | 0.05 | asserted 0.99 |
| s2 | For comparison, we consider two irrotational equal mass (M=1.35 M_sol) and unequal mass (M=1.29,1.42 M_sol) BNS models using the APR4 EOS, which result in a supramassive merger remnant. | method 0.90 | 0.89 | 0.03 | asserted 0.99 |
| s3 | We present visualizations of the fluid flow and temperature distribution and find a strong impact of the spin on vortex structure and nonaxisymmetric deformation. | result 0.96 | 0.97 | 0.26 | asserted 1.00 |
| s4 | We compute the radial mass distribution and the rotation profile in the equatorial plane using recently developed measures independent of spatial gauge, revealing slowly rotating cores that can be well approximated by the cores of spherical stars. | result 0.79 | 0.97 | 0.16 | asserted 0.98 |
| s5 | We also study the influence of the spin on the inspiral phase and the gravitational wave (GW) signal. | contribution 1.00 | 0.89 | 0.05 | asserted 0.64 |
| s6 | Using a newly developed analysis method, we further show that gravitational waveforms from BNS mergers can exhibit one or more phase jumps after merger, which occur together with minima of the strain amplitude. | result 0.77 | 0.96 | 0.22 | asserted 0.98 |
| s7 | We provide a natural explanation in terms of the remnant's quadrupole moment, and show that cancellation effects due to phase jumps can have a strong impact on the GW power spectrum. | interpretation 0.92 | 0.95 | 0.20 | asserted 0.99 |
| s8 | Finally, we discuss the impact of the spin on the amount of ejected matter. | contribution 0.91 | 0.79 | 0.08 | unclear 0.83 |
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The paper
Original abstract
We present general relativistic numerical simulations of binary neutron star (BNS) mergers with different initial spin configurations. We focus on models with stars of mass 1.4 M_sol each, which employ the equation of state (EOS) by Shen, Horowitz, and Teige, and which result in stable NSs as merger remnants. For comparison, we consider two irrotational equal mass (M=1.35 M_sol) and unequal mass (M=1.29,1.42 M_sol) BNS models using the APR4 EOS, which result in a supramassive merger remnant. We present visualizations of the fluid flow and temperature distribution and find a strong impact of the spin on vortex structure and nonaxisymmetric deformation. We compute the radial mass distribution and the rotation profile in the equatorial plane using recently developed measures independent of spatial gauge, revealing slowly rotating cores that can be well approximated by the cores of spherical stars. We also study the influence of the spin on the inspiral phase and the gravitational wave (GW) signal. Using a newly developed analysis method, we further show that gravitational waveforms from BNS mergers can exhibit one or more phase jumps after merger, which occur together with minima of the strain amplitude. We provide a natural explanation in terms of the remnant's quadrupole moment, and show that cancellation effects due to phase jumps can have a strong impact on the GW power spectrum. Finally, we discuss the impact of the spin on the amount of ejected matter.
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References
How the literature uses it
21 arXiv papers cite this in 41 sentences
Papers citing it · 25 sentences without a confident label
Uses its method or tool 3 papers
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The precession cones for the individual stars are based on the quasi-local spin measurement introduced in [ref] [equation] evaluated on coordinate spheres with radius $r_s$ around the NSs. $φ^li = ϵ^l i k x_k$ defines the approximate rotational Killing vectors in Cartesian coordinates ($φ^l1,φ^l2,φ^l3$), $K_ij$ denotes the extrinsic curvature, $γ^ij$ is the inverse 3-metric, and $n_i = (x_i-x_i^NS)/r$ is the normal vector with respect to the center of the NS, see also [ref] .
Numerical Relativity Simulations of Precessing Binary Neutron Star Mergers · Precession Dynamics · 0.99
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For further details of the method, we refer to [ref] .
General relativistic magnetohydrodynamic simulations of binary neutron star mergers forming a long-lived neutron star · GW emission · 0.94
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As a quantitative measure for the radial mass distribution, we compute baryonic mass and proper volume enclosed in the surfaces of constant mass density, obtaining a gauge independent mass-inside-volume relation (see [ref] ).
First 100 ms of a long-lived magnetized neutron star formed in a binary neutron star merger · Remnant structure and rotation profile · 0.93
Compares with it 3 papers
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For the early postmerger phase, up to around $30$ ms after the merger, we confirm the results of earlier numerical studies [ref] , which observe a gravitational wave consisting of a single component with a frequency equal to twice the maximum rotation rate.
First 100 ms of a long-lived magnetized neutron star formed in a binary neutron star merger · Gravitational waves and remnant oscillations · 0.85
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This observation is in agreement with, e.g, [ref] , while [ref] point out that in some cases anti-aligned setups can eject more massive ejecta.
High-accuracy simulations of highly spinning binary neutron star systems · Ejecta and Remnant properties · 0.81
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Our findings are similar to the results obtained for different models in [ref] .
General relativistic magnetohydrodynamic simulations of binary neutron star mergers forming a long-lived neutron star · Rotation profile and remnant structure · 1.00
Cites it as support 1 paper
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This indicates that the dominant ejecta mechanism are shocks produced during the merger of the two stars, see also [ref] .
Numerical Relativity Simulations of Precessing Binary Neutron Star Mergers · Ejecta · 0.96
Cites it as background 6 papers
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While initially most numerical relativity (NR) studies have neglected spin effects, there has been a noticeable advancement over the last few years in which different groups studied BNS configurations in which the individual NSs are spinning, see Refs. [ref] .
High-accuracy simulations of highly spinning binary neutron star systems · Introduction · 0.89
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Simulations of spinning binary NSs are currently under way by several groups, see, e.g., [ref] for quasicircular mergers with constraint-satisfying, quasiequilibrium initial data, and [ref] where the initial data are constraint violating and not in equilibrium.
Binary neutron star mergers: Effects of spin and post-merger dynamics · Introduction · 0.90
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In this article, we focus on the BH formation, but we refer to, e.g., Refs. [ref] for a selection of numerical-relativity studies that investigated the influence of different system parameters on the binary dynamics.
Black-hole formation in binary neutron star mergers: The impact of spin on the prompt-collapse scenario · Black Hole Formation and Maximum Density · 1.00
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