Simulating binary neutron stars: Dynamics and gravitational waves

Anderson, Matthew; Hirschmann, Eric; Lehner, Luis; Liebling, Steven L.; Motl, Patrick M.; Neilsen, David; Palenzuela, Carlos; Tohline, J. E.

doi:10.1103/physrevd.77.024006

Cited by 147 publications

(156 citation statements)

References 54 publications

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“…We note, however, that the initial data used by Shibata et [27], whereas the eccentricities of the CTS initial data are < ∼ 0.015 according to a post-Newtonian analysis [30]. We point out that a quasi-circular orbit is more realistic because gravitational radiation would have circularized the orbit long before the binary separation reaches a few NS radii.…”

Section: Introductionmentioning

confidence: 90%

“…Recently, Anderson et al have used their code to study the coalescence of both unmagnetized and magnetized NSNSs [27,28]. In the unmagnetized cases, they find an initial configuration in [27] that leads to prompt collapse to a black hole following the merger.…”

Section: Introductionmentioning

confidence: 99%

“…In the unmagnetized cases, they find an initial configuration in [27] that leads to prompt collapse to a black hole following the merger. The total (baryon) rest mass of their initial configuration is M 0 ≈ 1.03M…”

Section: Introductionmentioning

confidence: 99%

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General relativistic simulations of magnetized binary neutron star mergers

et al. 2008

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Binary neutron stars (NSNS) are expected to be among the leading sources of gravitational waves observable by ground-based laser interferometers and may be the progenitors of short-hard gamma ray bursts. We present a series of general relativistic NSNS coalescence simulations both for unmagnetized and magnetized stars. We adopt quasiequilibrium initial data for circular, irrotational binaries constructed in the conformal thin-sandwich (CTS) framework. We adopt the BSSN formulation for evolving the metric and a high-resolution shock-capturing scheme to handle the magnetohydrodynamics. Our simulations of unmagnetized binaries agree with the results of Shibata, Taniguchi and Uryū [1]. In cases in which the mergers result in a prompt collapse to a black hole, we are able to use puncture gauge conditions to extend the evolution and determine the mass of the material that forms a disk. We find that the disk mass is less than 2% of the total mass in all cases studied. We then add a small poloidal magnetic field to the initial configurations and study the subsequent evolution. For cases in which the remnant is a hypermassive neutron star, we see measurable differences in both the amplitude and phase of the gravitational waveforms following the merger. For cases in which the remnant is a black hole surrounded by a disk, the disk mass and the gravitational waveforms are about the same as the unmagnetized cases. Magnetic fields substantially affect the long-term, secular evolution of a hypermassive neutron star (driving 'delayed collapse') and an accretion disk around a nascent black hole.

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Section: Introductionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

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General relativistic simulations of magnetized binary neutron star mergers

et al. 2008

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“…For example, numerical relativity has provided vital information regarding the kick or recoil in astrophysical mergers [14,15,16,17,18,19,20,21,22,23], simulations of spin flip and precession phenomena [15,24] and the interpretation of gravitational waveforms to be observed in the future [25,26,27,28,29,30]. See also [31,32,33,34,35] for binary simulations involving neutron stars. This progress has come timely, as earthbound gravitational wave detectors LIGO, VIRGO, GEO600 and TAMA [36,37,38,39] are now collecting data at or near the design sensitivity.…”

Section: Introductionmentioning

confidence: 99%

Black-hole binary simulations: The mass ratio10∶1

2009

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We present the first numerical simulations of an initially non-spinning black-hole binary with mass ratio as large as 10 : 1 in full general relativity. The binary completes approximately 3 orbits prior to merger and radiates (0.415 ± 0.017) % of the total energy and (12.48 ± 0.62) % of the initial angular momentum in the form of gravitational waves. The single black hole resulting from the merger acquires a kick of (66.7 ± 3.3) km/s relative to the original center of mass frame. The resulting gravitational waveforms are used to validate existing formulas for the recoil, final spin and radiated energy over a wider range of the symmetric mass ratio parameter η = M1M2/(M1 + M2) 2 than previously possible. The contributions of ℓ > 2 multipoles are found to visibly influence the gravitational wave signal obtained at fixed inclination angles.

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“…Most of that effort was aimed at the evolution of compact binaries, sources of waves potentially observable by those detectors. Binary neutron stars were the first to be successfully evolved in a fully relativistic framework, and have been studied regularly over the last eight years [3,4,5,6,7,8,9]. Evolutions of binary black holes (BBH) followed a few years later [10,11,12], and continue to be an extraordinarily active area of research (see [13] and references therein).…”

Section: Introductionmentioning

confidence: 99%

Initial data for black hole–neutron star binaries: A flexible, high-accuracy spectral method

et al. 2008

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We present a new numerical scheme to solve the initial value problem for black hole-neutron star binaries. This method takes advantage of the flexibility and fast convergence of a multidomain spectral representation of the initial data to construct high-accuracy solutions at a relatively low computational cost. We provide convergence tests of the method for both isolated neutron stars and irrotational binaries. In the second case, we show that we can resolve the small inconsistencies that are part of the quasiequilibrium formulation, and that these inconsistencies are significantly smaller than observed in previous works. The possibility of generating a wide variety of initial data is also demonstrated through two new configurations inspired by results from binary black holes. First, we show that choosing a modified Kerr-Schild conformal metric instead of a flat conformal metric allows for the construction of quasiequilibrium binaries with a spinning black hole. Second, we construct binaries in low-eccentricity orbits, which are a better approximation to astrophysical binaries than quasiequilibrium systems.

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Simulating binary neutron stars: Dynamics and gravitational waves

Cited by 147 publications

References 54 publications

General relativistic simulations of magnetized binary neutron star mergers

General relativistic simulations of magnetized binary neutron star mergers

Black-hole binary simulations: The mass ratio10∶1

Initial data for black hole–neutron star binaries: A flexible, high-accuracy spectral method

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