Bowen-York-type initial data for binaries with neutron stars

Clark, Michael; Laguna, Pablo

doi:10.1103/physrevd.94.064058

Cited by 9 publications

(19 citation statements)

References 47 publications

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“…In [10], the constraint violating data was evolved, while in [15,16] the constraint equations were solved again after the superposition. In [17], the Bowen-York formalism for BBHs was extended to BNS. In [8,9], a rotational velocity fields was added manually to irrotational binary models and the constraint violating initial data was evolved with a constraint-damping formalism.…”

Section: Introductionmentioning

confidence: 99%

Structure of stable binary neutron star merger remnants: Role of initial spin

et al. 2017

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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 ⊙ 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 ¼ 1.35 M ⊙ ) and unequal mass (M ¼ 1.29, 1.42 M ⊙ ) 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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Section: Introductionmentioning

confidence: 99%

Structure of stable binary neutron star merger remnants: Role of initial spin

et al. 2017

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“…We will briefly review the approach we introduced in Ref. [30] to construct initial data for binaries with NS companions. Under the 3+1 decomposition of the Einstein equations, initial data consist of the spatial metric γ ij of the constant time initial hypersurface, the extrinsic curvature K ij in this hypersurface, and the projections…”

Section: Initial Datamentioning

confidence: 99%

“…In Ref. [30], we followed Bowen's approach [34] to construct solutions to the momentum constraint that represent NSs. The solutions assume spherically symmetric sources and are given by…”

Section: Initial Datamentioning

confidence: 99%

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Black Hole - Neutron Star Binary Mergers: The Imprint of Tidal Deformations and Debris

Khamesra,

Gracia-Linares,

Laguna

2021

Preprint

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The increase in the sensitivity of gravitational wave interferometers will bring additional detections of binary black hole and double neutron star mergers. It will also very likely add many merger events of black hole -neutron star binaries. Distinguishing mixed binaries from binary black holes mergers for high mass ratios could be challenging because in this situation the neutron star coalesces with the black hole without experiencing significant disruption. To investigate the transition of mixed binary mergers into those behaving more like binary black hole coalescences, we present results from merger simulations for different mass ratios. We show how the degree of deformation and disruption of the neutron star impacts the inspiral and merger dynamics, the properties of the final black hole, the accretion disk formed from the circularization of the tidal debris, the gravitational waves, and the strain spectrum and mismatches. The results also show the effectiveness of the initial data method that generalizes the Bowen-York initial data for black hole punctures to the case of binaries with neutron star companions.

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“…Numerical General Relativity played a crucial role in the analysis of the detected signals. BBH and BNS simulations were involved in the construction of the phenomenological and effective-one-body waveform models used in the analysis [8]. Catalogs of parameters, initial data and waveforms have been published [9].…”

Section: Introductionmentioning

confidence: 99%

RIO: a new computational framework for accurate initial data of binary black holes

et al. 2018

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We present a computational framework (Rio) in the ADM 3+1 approach for numerical relativity. This work enables us to carry out high resolution calculations for initial data of two arbitrary black holes. We use the transverse conformal treatment, the Bowen-York and the puncture methods. For the numerical solution of the Hamiltonian constraint we use the domain decomposition and the spectral decomposition of Galerkin-Collocation. The nonlinear numerical code solves the set of equations for the spectral modes using the standard Newton-Raphson method, LU decomposition and Gaussian quadratures. We show the convergence of the Rio code. This code allows for easy deployment of large calculations. We show how the spin of one of the black holes is manifest in the conformal factor.

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Bowen-York-type initial data for binaries with neutron stars

Cited by 9 publications

References 47 publications

Structure of stable binary neutron star merger remnants: Role of initial spin

Structure of stable binary neutron star merger remnants: Role of initial spin

Black Hole - Neutron Star Binary Mergers: The Imprint of Tidal Deformations and Debris

RIO: a new computational framework for accurate initial data of binary black holes

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