Towards a realistic neutron star binary inspiral: Initial data and multiple orbit evolution in full general relativity

Miller, Mark; Gressman, Philip T.; Suen, Wai-Mo

doi:10.1103/physrevd.69.064026

Cited by 65 publications

(144 citation statements)

References 50 publications

(72 reference statements)

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“…However, as the separation between the two compact objects decreases, this approximation becomes less accurate and eventually breaks [21,22], forcing the use of fully dynamical simulations. A first step in this direction within a relativistic context has been made recently within the characteristic formulation of Einstein equations [23].…”

Section: Introductionmentioning

confidence: 99%

Numerical evolutions of a black hole-neutron star system in full general relativity: Head-on collision

Löffler

Rezzolla²,

Ansorg³

2006

Phys. Rev. D

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We present the first simulations in full general relativity of the head-on collision between a neutron star and a black hole of comparable mass. These simulations are performed through the solution of the Einstein equations combined with an accurate solution of the relativistic hydrodynamics equations via high-resolution shock-capturing techniques. The initial data is obtained by following the YorkLichnerowicz conformal decomposition with the assumption of time symmetry. Unlike other relativistic studies of such systems, no limitation is set for the mass ratio between the black hole and the neutron star, nor on the position of the black hole, whose apparent horizon is entirely contained within the computational domain. The latter extends over 400M and is covered with six levels of fixed mesh refinement. Concentrating on a prototypical binary system with mass ratio 6, we find that although a tidal deformation is evident the neutron star is accreted promptly and entirely into the black hole. While the collision is completed before 300M, the evolution is carried over up to 1700M, thus providing time for the extraction of the gravitational-wave signal produced and allowing for a first estimate of the radiative efficiency of processes of this type.

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Section: Introductionmentioning

confidence: 99%

Numerical evolutions of a black hole-neutron star system in full general relativity: Head-on collision

Löffler

Rezzolla²,

Ansorg³

2006

Phys. Rev. D

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“…For many years, the fully general relativistic (GR) simulations for the merger of binary neutron stars had been performed adopting an ideal equation of state (EOS) P = (Γ−1)ρε where P , ρ, ε, and Γ are pressure, rest-mass density, specific internal energy, and adiabatic constant [12,13,17,18,19]. However, simulations with realistic EOSs are necessary for quantitative understanding for the merger.…”

Section: Introductionmentioning

confidence: 99%

“…Over the last several years, numerical methods for solving coupled equations of the Einstein and hydrodynamic equations have been developed (e.g., [11,12,13,14,15,16,17,18,19,20,21]) and now such simulations are feasible with an accuracy high enough for yielding scientific results (e.g., [17,21]). …”

Section: Introductionmentioning

confidence: 99%

Merger of binary neutron stars to a black hole: Disk mass, short gamma-ray bursts, and quasinormal mode ringing

2006

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Three-dimensional simulations for the merger of binary neutron stars are performed in the framework of full general relativity. We pay particular attention to the black hole formation case and to the resulting mass of the surrounding disk for exploring possibility for formation of the central engine of short-duration gamma-ray bursts (SGRBs). Hybrid equations of state are adopted mimicking realistic, stiff nuclear equations of state (EOSs), for which the maximum allowed gravitational mass of cold and spherical neutron stars, M sph , is larger than 2M⊙. Such stiff EOSs are adopted motivated by the recent possible discovery of a heavy neutron star of mass ∼ 2.1 ± 0.2M⊙. For the simulations, we focus on binary neutron stars of the ADM mass M > ∼ 2.6M⊙. For an ADM mass larger than the threshold mass M thr , the merger results in prompt formation of a black hole irrespective of the mass ratio QM with 0.65 < ∼ QM ≤ 1. The value of M thr depends on the EOSs and is approximately written as 1.3-1.35M sph for the chosen EOSs. For the black hole formation case, we evolve the spacetime using a black hole excision technique and determine the mass of a quasistationary disk surrounding the black hole. The disk mass steeply increases with decreasing the value of QM for given ADM mass and EOS. This suggests that a merger with small value of QM is a candidate for producing central engine of SGRBs. For M < M thr , the outcome is a hypermassive neutron star of a large ellipticity. Because of the nonaxisymmetry, angular momentum is transported outward. If the hypermassive neutron star collapses to a black hole after the longterm angular momentum transport, the disk mass may be > ∼ 0.01M⊙ irrespective of QM . Gravitational waves are computed in terms of a gauge-invariant wave extraction technique. In the formation of the hypermassive neutron star, quasiperiodic gravitational waves of frequency between 3 and 3.5 kHz are emitted irrespective of EOSs. The effective amplitude of gravitational waves can be > ∼ 5 × 10 −21 at a distance of 50 Mpc, and hence, it may be detected by advanced laser-interferometers. For the black hole formation case, the black hole excision technique enables a longterm computation and extraction of ring-down gravitational waves associated with a black hole quasinormal mode. It is found that the frequency and amplitude are ≈ 6.5-7 kHz and ∼ 10 −22 at a distance of 50 Mpc for the binary of mass M ≈ 2.7-2.9M⊙.

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“…In the past several years, this field has been extensively developed (e.g., [1][2][3][4][5][6][7]) and, as a result, now it is feasible to perform accurate simulations of such general relativistic phenomena for yielding scientific results (e.g., [6][7][8][9] for our latest results). For example, with the current implementation, radiation reaction of gravitational waves in the merger of binary neutron stars can be taken into account within ∼ 1% error in an appropriate computational setting [6,7].…”

Section: Introductionmentioning

confidence: 99%

Magnetohydrodynamics in full general relativity: Formulation and tests

2005

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A new implementation for magnetohydrodynamics (MHD) simulations in full general relativity (involving dynamical spacetimes) is presented. In our implementation, Einstein's evolution equations are evolved by a BSSN formalism, MHD equations by a high-resolution central scheme, and induction equation by a constraint transport method. We perform numerical simulations for standard test problems in relativistic MHD, including special relativistic magnetized shocks, general relativistic magnetized Bondi flow in stationary spacetime, and a longterm evolution for self-gravitating system composed of a neutron star and a magnetized disk in full general relativity. In the final test, we illustrate that our implementation can follow winding-up of the magnetic field lines of magnetized and differentially rotating accretion disks around a compact object until saturation, after which magnetically driven wind and angular momentum transport inside the disk turn on.04.25. Dm, 04.40.Nr, 47.75.+f, 95.30.Qd

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Towards a realistic neutron star binary inspiral: Initial data and multiple orbit evolution in full general relativity

Cited by 65 publications

References 50 publications

Numerical evolutions of a black hole-neutron star system in full general relativity: Head-on collision

Numerical evolutions of a black hole-neutron star system in full general relativity: Head-on collision

Merger of binary neutron stars to a black hole: Disk mass, short gamma-ray bursts, and quasinormal mode ringing

Magnetohydrodynamics in full general relativity: Formulation and tests

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