Binary neutron stars with arbitrary spins in numerical relativity

Tacik, Nick; Foucart, François; Pfeiffer, Harald P.; Haas, Roland; Ossokine, S.; Kaplan, Jeff; Muhlberger, Curran D.; Duez, Matthew D.; Kidder, Lawrence E.; Scheel, Mark A.; Szilágyi, Béla

doi:10.1103/physrevd.92.124012

Cited by 56 publications

(65 citation statements)

References 91 publications

(192 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Although the first initial data for neutron-star binaries has been computed for corotating systems [40], the large majority of the simulations performed to date has used irrotational configurations, since neutron star viscosity is believed to be too small to tidally lock the two stars prior to merger [41,42]. At the same time, the most advanced efforts over the last couple of years have been concentrated on approaches to reduce the eccentricity of the orbits or to produce binary systems with arbitrary neutron star spins [32,36,[43][44][45][46][47][48][49].…”

Section: Introductionmentioning

confidence: 99%

Initial-data contribution to the error budget of gravitational waves from neutron-star binaries

et al. 2016

View full text Add to dashboard Cite

As numerical calculations of inspiralling neutron-star binaries reach values of accuracy that are comparable with those of binary black holes, a fine budgeting of the various sources of error becomes increasingly important. Among such sources, the initial data is normally not accounted for, the rationale being that the error on the initial spacelike hypersurface is always far smaller than the one gained during the evolution. We here consider critically this assumption and perform a comparative analysis of the gravitational waveforms relative to essentially the same physical binary configuration when computed with two different initial-data codes, and then evolved with the same evolution code. More specifically, we consider the evolution of irrotational neutron-star binaries computed either with the pseudo-spectral code LORENE, or with the newly developed finite-difference code COCAL; both sets of initial data are subsequently evolved with the high-order evolution code WHISKYTHC. In this way we find that despite the initial data shows global (local) differences that are 0.02% (1%), the gravitationalwave phase at the merger time differs by ∼ 0.5 radians after ∼ 3 orbits, a surprisingly large value. Our results highlight the highly nonlinear impact that errors in the initial data can have on the subsequent evolution and the importance of using exactly the same initial data when comparative studies are done.

show abstract

Section: Introductionmentioning

confidence: 99%

Initial-data contribution to the error budget of gravitational waves from neutron-star binaries

et al. 2016

View full text Add to dashboard Cite

show abstract

“…We list below only a few examples over the past year (since 2015). Recent applications of WENO schemes can be found in the simulations of astrophysics and geophysics [55,83,137,140,162,172,215,223], atmospheric and climate science [70,181,225], batch chromatographic separation [101], biomolecular solvation [286], bubble clusters in fluids [222], combustion [11,15,24,164,214,268], detonation waves [92,114,145,233], elastic-plastic solids [173], flame structure [261], granular gas [3], hypersonic flows [109], infectious disease models [209], laser welding [174], magnetohydrodynamics [20,166], mathematical finance for solving the Black-Scholes equation [90], multiphase and multispecies flows [13,91,108,110,159,160,239], networks and blood flows [168], ocean waves [28,125], oil storage process [196], rarefi...…”

Section: Finite Difference and Finite Volume Weno Schemesmentioning

confidence: 99%

High order WENO and DG methods for time-dependent convection-dominated PDEs: A brief survey of several recent developments

Shu

2016

Journal of Computational Physics

164

View full text Add to dashboard Cite

For solving time-dependent convection-dominated partial differential equations (PDEs), which arise frequently in computational physics, high order numerical methods, including finite difference, finite volume, finite element and spectral methods, have been undergoing rapid developments over the past decades. In this article we give a brief survey of two selected classes of high order methods, namely the weighted essentially non-oscillatory (WENO) finite difference and finite volume schemes and discontinuous Galerkin (DG) finite element methods, emphasizing several of their recent developments: bound-preserving limiters for DG, finite volume and finite difference schemes, which address issues in robustness and accuracy; WENO limiters for DG methods, which address issues in non-oscillatory performance when there are strong shocks, and inverse Lax-Wendroff type boundary treatments for finite difference schemes, which address issues in solving complex geometry problems using Cartesian meshes.

show abstract

“…The same set of equations discussed above has also been used in [130,131]. Notice, however, that [130] erroneously assumes £ ξ p = 0 = £ V w .…”

Section: Binary Neutron Stars With Arbitrary Spinsmentioning

confidence: 99%

“…Notice, however, that in [135] and [126] only quasi-circular orbits are considered and Ω and v r are directly adjusted. Similarly [131] considers quasi-circular orbits using the methods for spinning stars discussed above and also directly adjusts Ω and v r .…”

Section: General Orbits and Low Eccentricity Orbitsmentioning

confidence: 99%

The initial value problem as it relates to numerical relativity

Tichy

2016

Rep. Prog. Phys.

View full text Add to dashboard Cite

Abstract.Spacetime is foliated by spatial hypersurfaces in the 3+1 split of General Relativity. The initial value problem then consists of specifying initial data for all fields on one such a spatial hypersurface, such that the subsequent evolution forward in time is fully determined. On each hypersurface the 3-metric and extrinsic curvature describe the geometry. Together with matter fields such as fluid velocity, energy density and rest mass density, the 3-metric and extrinsic curvature then constitute the initial data. There is a lot of freedom in choosing such initial data. This freedom corresponds to the physical state of the system at the initial time. At the same time the initial data have to satisfy the Hamiltonian and momentum constraint equations of General Relativity and can thus not be chosen completely freely. We discuss the conformal transverse traceless and conformal thin sandwich decompositions that are commonly used in the construction of constraint satisfying initial data. These decompositions allow us to specify certain free data that describe the physical nature of the system. The remaining metric fields are then determined by solving elliptic equations derived from the constraint equations. We describe initial data for single black holes and single neutron stars, and how we can use conformal decompositions to construct initial data for binaries made up of black holes or neutron stars. Orbiting binaries will emit gravitational radiation and thus lose energy. Since the emitted radiation tends to circularize the orbits over time, one can thus expect that the objects in a typical binary move on almost circular orbits with slowly shrinking radii. This leads us to the concept of quasi-equilibrium which essentially assumes that time derivatives are negligible in corotating coordinates, for binaries on almost circular orbits. We review how quasi-equilibrium assumptions can be used to make physically well motivated approximations that simplify the elliptic equations we have to solve.

show abstract

Binary neutron stars with arbitrary spins in numerical relativity

Cited by 56 publications

References 91 publications

Initial-data contribution to the error budget of gravitational waves from neutron-star binaries

Initial-data contribution to the error budget of gravitational waves from neutron-star binaries

High order WENO and DG methods for time-dependent convection-dominated PDEs: A brief survey of several recent developments

The initial value problem as it relates to numerical relativity

Contact Info

Product

Resources

About