Black hole-neutron star binaries in general relativity: Quasiequilibrium formulation

Baumgarte, Thomas W.; Skoge, Monica; Shapiro, Stuart L.

doi:10.1103/physrevd.70.064040

Cited by 38 publications

(60 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This study was partly motivated by our curiousity in the behavior of the bare mass along sequences of constant irreducible mass (compare the discussion in Ref. [42], in particular endnote [35] of that article.) Moreover, our solutions provide approximate values for the conformal factor and the extrinsic curvature together with the above global quantities, thereby specifying complete sets of initial data describing binary black holes in approximate quasicircular orbit.…”

Section: Discussionmentioning

confidence: 99%

Approximate initial data for binary black holes

2006

Self Cite

View full text Add to dashboard Cite

We construct approximate analytical solutions to the constraint equations of general relativity for binary black holes of arbitrary mass ratio in quasicircular orbit. We adopt the puncture method to solve the constraint equations in the transverse-traceless decomposition and consider perturbations of Schwarzschild black holes caused by boosts and the presence of a binary companion. A superposition of these two perturbations then yields approximate, but fully analytic binary black hole initial data that are accurate to first order in the inverse of the binary separation and the square of the black holes' momenta.

show abstract

Section: Discussionmentioning

confidence: 99%

Approximate initial data for binary black holes

2006

Self Cite

View full text Add to dashboard Cite

show abstract

“…More recently these studies have been improved with either the use of relativistic corrections to the Newtonian gravity in terms of pseudo-Newtonian potentials [19] or in general relativity but within a ''quasistationary'' approximation [20]. The latter assumes that the evolution of the binary system can be modeled through a sequence of quasistationary spacetimes, solutions of the Einstein equations.…”

Section: Introductionmentioning

confidence: 99%

“…Taking as initial data the one computed in Ref. [20], Faber et al have studied the final dynamics of the binary system using SPH techniques for the hydrodynamics and a conformally flat approximation to the Einstein equations. In these calculations the black hole is only included as a background metric in addition to the one of the neutron star and it is not included in the computational domain, thus limiting the investigation to rather large black hole-to-neutron star mass ratios.…”

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

View full text Add to dashboard Cite

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.

show abstract

“…Numerical relativity simulations of mixed black holeneutron star binaries are not as far advanced as those of black hole binaries or neutron star binaries. So far, fully relativistic, self-consistent studies exist for quasiequilibrium models [53,54,55] (see also [56]). The first fully self-consistent, dynamical simulations of the binary inspiral and the tidal disruption of the neutron star have been announced very recently [57] (see also [60] for simulations of extreme mass-ratio binaries within the so-called Wilson-Mathews approximation, which assumes that the spatial metric remains conformally flat).…”

Section: Black Hole-neutron Star Binariesmentioning

confidence: 99%

Learning about compact binary merger: The interplay between numerical relativity and gravitational-wave astronomy

et al. 2008

View full text Add to dashboard Cite

Activities in data analysis and numerical simulation of gravitational waves have to date largely proceeded independently. In this work we study how waveforms obtained from numerical simulations could be effectively used within the data analysis effort to search for gravitational waves from black hole binaries. We propose measures to quantify the accuracy of numerical waveforms for the purpose of data analysis and study how sensitive the analysis is to errors in the waveforms. We estimate that ∼ 100 templates (and ∼ 10 simulations with different mass ratios) are needed to detect waves from non-spinning binary black holes with total masses in the range 100M⊙ ≤ M ≤ 400M⊙ using initial LIGO. Of course, many more simulation runs will be needed to confirm that the correct physics is captured in the numerical evolutions. From this perspective, we also discuss sources of systematic errors in numerical waveform extraction and provide order of magnitude estimates for the computational cost of simulations that could be used to estimate the cost of parameter space surveys. Finally, we discuss what information from near-future numerical simulations of compact binary systems would be most useful for enhancing the detectability of such events with contemporary gravitational wave detectors and emphasize the role of numerical simulations for the interpretation of eventual gravitational-wave observations.

show abstract

Black hole-neutron star binaries in general relativity: Quasiequilibrium formulation

Cited by 38 publications

References 35 publications

Approximate initial data for binary black holes

Approximate initial data for binary black holes

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

Learning about compact binary merger: The interplay between numerical relativity and gravitational-wave astronomy

Contact Info

Product

Resources

About